146 results on '"V. A. Sergeev"'
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2. Ionospheric Electron Density and Conductance Changes in the Auroral Zone During Substorms
- Author
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M. A. Shukhtina, V. A. Sergeev, D. D. Rogov, Xiangning Chu, Yasunobu Ogawa, and N. A. Stepanov
- Subjects
Physics ,Geophysics ,Auroral zone ,Space and Planetary Science ,Ionospheric electron density ,Conductance ,Computational physics - Published
- 2021
3. Search for Transient Gravitational-wave Signals Associated with Magnetar Bursts during Advanced LIGO's Second Observing Run
- Author
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Abbott, B. P, Abbott, R, Abbott, T. D, Abraham, S, Acernese, F, Ackley, K, Adams, C, Adhikari, R. X, Adya, V. B, Affeldt, C, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O. D, Aiello, L, Ain, A, Ajith, P, Allen, G, Allocca, A, Aloy, M. A, Altin, P. A, Amato, A, Ananyeva, A, Anderson, S. B, Anderson, W. G, Angelova, V, S, Antier, S, Appert, S, Arai, K, Araya, M. C, Areeda, J. S, Arene, M, Arnaud, N, Ascenzi, S, Ashton, G, Aston, S. M, Astone, P, Aubin, F, Aufmuth, P, Aultoneal, K, Austin, C, Avendano, V and Avila-Alvarez, A, Babak, S, Bacon, P, Badaracco, F, Bader, M. K. M, Bae, S, Baker, P. T, Baldaccini, F, Ballardin, G, Ballmer, S. W, Banagiri, S, Barayoga, J. C, Barclay, S. E, Barish, B. C, Barker, D, Barkett, K, Barnum, S, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Bartos, I and Bassiri, R, Basti, A, Bawaj, M, Bayley, J. C, Bazzan, M, Becsy, B, Bejger, M, Belahcene, I and Bell, A. S., Beniwal, D, Berger, B. K, Bergmann, G, Bernuzzi, S, Bero, J. J, Berry, C. P. L, Bersanetti, D, Bertolini, A, Betzwieser, J, Bhandare, R, Bidler, J, Bilenko, I. A, Bilgili, S. A, Billingsley, G, Birch, J, Birney, R, Birnholtz, O, Biscans, S, Biscoveanu, S, Bisht, A, Bitossi, M, Bizouard, M. A, Blackburn, J. K, Blair, C. D, Blair, D. G, Blair, R. M, Bloemen, S, Bode, N, Boer, M, Boetzel, Y, Bogaert, G, Bondu, F, Bonilla, E, Bonnand, R, Booker, P, Boom, B. A, Booth, C. D, Bork, R, Boschi, V and Bose, Bossie, K, Bossilkov, V and Bosveld, J, Bouffanais, Y, Bozzi, A, Bradaschia, C, Brady, P. R, Bramley, A, Branchesi, M, Brau, J. E, Briant, T, Briggs, J. H, Brighenti, F, Brillet, A, Brinkmann, M, Brisson, V and Brockill, P, Brooks, A. F, Brown, D. D, Brunett, S, Buikema, A, Bulik, T, Bulten, H. J, Buonanno, A, Buskulic, D, Buy, C, Byer, R. L, Cabero, M, Cadonati, L, Cagnoli, G, Cahillane, C, Bustillo, Calderon and Callister, J., T. A., Calloni, E, Camp, J. B, Campbell, W. A, Canepa, M, Cannon, K. C, Cao, H, Cao, J, Capocasa, E, Carbognani, F, Caride, S, Carney, M. F, Carullo, G, Diaz, Casanueva and Casentini, J., C, Caudill, S, Cavaglia, M, Cavalier, F, Cavalieri, R, Cella, G, Cerda-Duran, P, Cerretani, G, Cesarini, E, Chaibi, O, Chakravarti, K, Chamberlin, S. J, Chan, M, Chao, S, Charlton, P, Chase, E. A, Chassande-Mottin, E, Chatterjee, D, Chaturvedi, M, Cheeseboro, B. D, Chen, H. Y, Chen, X, Chen, Y, Cheng, H-P and Cheong, C. K., Chia, H. Y, Chincarini, A, Chiummo, A, Cho, G, Cho, H. S, Cho, M, Christensen, N, Chu, Q, Chua, S, Chung, K. W, Chung, S, Ciani, G, Ciobanu, A. A, Ciolfi, R, Cipriano, F, Cirone, A, Clara, F, Clark, J. A, Clearwater, P, Cleva, F, Cocchieri, C, Coccia, E, Cohadon, P-F and Cohen, D, Colgan, R, Colleoni, M, Collette, C. G, Collins, C, Cominsky, L. R, Constancio Jr, M, Conti, L, Cooper, S. J, Corban, P, Corbitt, T. R, Cordero-Carrion, I and Corley, K. R., Cornish, N, Corsi, A, Cortese, S, Costa, C. A, Cotesta, R, Coughlin, M. W, Coughlin, S. B, Coulon, J-P and Countryman, S. T., Couvares, P, Covas, P. B, Cowan, E. E, Coward, D. M, Cowart, M. J, Coyne, D. C, Coyne, R, Creighton, J. D. E, Creighton, T. D, Cripe, J, Croquette, M, Crowder, S. G, Cullen, T. J, Cumming, A, Cunningham, L, Cuoco, E, Dal Canton, T, Dalya, G, Danilishin, S. L, Dantonio, S, Danzmann, K, Dasgupta, A, Costa, Da Silva and Datrier, C. F., L. E. H., Dattilo, V and Dave, I and Davier, M, Davis, D, Daw, E. J, Debra, D, Deenadayalan, M, Degallaix, J, De Laurentis, M, Deleglise, S, Del Pozzo, W, Demarchi, L. M, Demos, N, Dent, T, De Pietri, R, Derby, J, De Rosa, R, De Rossi, C, Desalvo, R, de Varona, O, Dhurandhar, S, Diaz, M. C, Dietrich, T, Di Fiore, L, Di Giovanni, M, Di Girolamo, T, Di Lieto, A, Ding, B, Di Pace, S, Palma, Di, I and Di Renzo, F, Dmitriev, A, Doctor, Z, Donovan, F, Dooley, K. L, Doravari, S, Dorrington, I and Downes, T. P., Drago, M, Driggers, J. C, Du, Z, Ducoin, J-G and Dupej, Dwyer, S. E, Easter, P. J, Edo, T. B, Edwards, M. C, Effler, A, Ehrens, P, Eichholz, J, Eikenberry, S. S, Eisenmann, M, Eisenstein, R. A, Essick, R. C, Estelles, H, Estevez, D, Etienne, Z. B, Etzel, T, Evans, M, Evans, T. M, Fafone, V and Fair, H, Fairhurst, S, Fan, X, Farinon, S, Farr, B, Farr, W. M, Fauchon-Jones, E. J, Favata, M, Fays, M, Fazio, M, Fee, C, Feicht, J, Fejer, M. M, Feng, F, Fernandez-Galiana, A, Ferrante, I and Ferreira, E. C., Ferreira, T. A, Ferrini, F, Fidecaro, F, Fiori, I and Fiorucci, Fishbach, M, Fisher, R. P, Fishner, J. M, Fitz-Axen, M, Flaminio, R, Fletcher, M, Flynn, E, Fong, H, Font, J. A, Forsyth, P. W. F, Fournier, J-D and Frasca, Frasconi, F, Frei, Z, Freise, A, Frey, R, Frey, V and Fritschel, Frolov, V. V, Fulda, P, Fyffe, M, Gabbard, H. A, Gadre, B. U, Gaebel, S. M, Gair, J. R, Gammaitoni, L, Ganija, M. R, Gaonkar, S. G, Garcia, A, Garcia-Quiros, C, Garufi, F, Gateley, B, Gaudio, S, Gaur, G, Gayathri, V and Gemme, G, Genin, E, Gennai, A, George, D, George, J, Gergely, L, Germain, V and Ghonge, Ghosh, Abhirup and Ghosh, Archisman and Ghosh, Giacomazzo, B, Giaime, J. A, Giardina, K. D, Giazotto, A, Gill, K, Giordano, G, Glover, L, Godwin, P, Goetz, E, Goetz, R, Goncharov, B, Gonzalez, G, Castro, Gonzalez and Gopakumar, J. M., Gorodetsky, M. L, Gossan, S. E, Gosselin, M, Gouaty, R, Grado, A, Graef, C, Granata, M, Grant, A, Gras, S, Grassia, P, Gray, C, Gray, R, Greco, G, Green, A. C, Green, R, Gretarsson, E. M, Groot, P, Grote, H, Grunewald, S, Gruning, P, Guidi, G. M, Gulati, H. K, Guo, Y, Gupta, A, Gupta, M. K, Gustafson, E. K, Gustafson, R, Haegel, L, Halim, O, Hall, B. R, Hall, E. D, Hamilton, E. Z, Hammond, G, Haney, M, Hanke, M. M, Hanks, J, Hanna, C, Hannuksela, O. A, Hanson, J, Hardwick, T, Haris, K, Harms, J, Harry, G. M, Harry, I. W, Haster, C-J and Haughian, K, Hayes, F. J, Healy, J, Heidmann, A, Heintze, M. C, Heitmann, H, Hello, P, Hemming, G, Hendry, M, Heng, I. S, Hennig, J, Heptonstall, A. W, Vivanco, Francisco Hernandez and Heurs, Hild, S, Hinderer, T, Hoak, D, Hochheim, S, Hofman, D, Holgado, A. M, Holland, N. A, Holt, K, Holz, D. E, Hopkins, P, Horst, C, Hough, J, Howell, E. J, Hoy, C. G, Hreibi, A, Huerta, E. A, Huet, D, Hughey, B, Hulko, M, Husa, S, Huttner, S. H, Huynh-Dinh, T, Idzkowski, B, Iess, A, Ingram, C, Inta, R, Intini, G, Irwin, B, Isa, H. N, Isac, J-M and Isi, Iyer, B. R, Izumi, K, Jacqmin, T, Jadhav, S. J, Jani, K, Janthalur, N. N, Jaranowski, P, Jenkins, A. C, Jiang, J, Johnson, D. S, Jones, A. W, Jones, I, Jones, R, Jonker, R. J. G, Ju, L, Junker, J, Kalaghatgi, Kalogera, V and Kamai, B, Kandhasamy, S, Kang, G, Kanner, J. B, Kapadia, S. J, Karki, S, Karvinen, K. S, Kashyap, R, Kasprzack, M, Katsanevas, S, Katsavounidis, E, Katzman, W, Kaufer, S, Kawabe, K, Keerthana, N, Kefelian, F, Keitel, D, Kennedy, R, Key, J. S, Khalili, F. Y, Khan, H, Khan, I and Khan, Khan, Z, Khazanov, E. A, Khursheed, M, Kijbunchoo, N, Kim, Chunglee and Kim, J. C., Kim, K, Kim, W, Kim, W. S, Y-M and Kimball, King, E. J, King, P. J, Kinley-Hanlon, M, Kirchhoff, R, Kissel, J. S, Kleybolte, L, Klika, J. H, Klimenko, S, Knowles, T. D, Koch, P, Koehlenbeck, S. M, Koekoek, G, Koley, S, Kondrashov, V and Kontos, Koper, N, Korobko, M, Korth, W. Z, Kowalska, I and Kozak, D. B., Kringel, V and Krishnendu, Krlak, A, Kuehn, G, Kumar, A, Kumar, P, Kumar, R, Kumar, S, Kuo, L, Kutynia, A, Kwang, S, Lackey, B. D, Lai, K. H, Lam, T. L, Landry, M, Lane, B. B, Lang, R. N, Lange, J, Lantz, B, Lanza, R. K, Lartaux-Vollard, A, Lasky, P. D, Laxen, M, Lazzarini, A, Lazzaro, C, Leaci, P, Leavey, S, Lecoeuche, Y. K, Lee, C. H, Lee, H. K, Lee, H. M, Lee, H. W, Lee, J, Lee, K, Lehmann, J, Lenon, A, Leroy, N, Letendre, N, Levin, Y, Li, J, K. J. L, Li, T. G. F, Li, Li, X, Lin, F, Linde, F, Linker, S. D, Littenberg, T. B, Liu, J, Liu, X, R. K. L, Lo, Lockerbie, N. A, London, L. T, Longo, A, Lorenzini, M, Loriette, V and Lormand, Losurdo, G, Lough, J. D, Lousto, C. O, Lovelace, G, Lower, M. E, Lueck, H, Lumaca, D, Lundgren, A. P, Lynch, R, Ma, Y, Macas, R, Macfoy, S, Macinnis, M, Macleod, D. M, Macquet, A, Magana-Sandoval, F, Zertuche, Magana and Magee, L., R. M., Majorana, E, Maksimovic, I and Malik, Man, N, Mandic, V and Mangano, V and Mansell, G. L., Manske, M, Mantovani, M, Marchesoni, F, Marion, F, Marka, S, Marka, Z, Markakis, C, Markosyan, A. S, Markowitz, A, Maros, E, Marquina, A, Marsat, S, Martelli, F, Martin, I. W, Martin, R. M, Martynov, Mason, K, Massera, E, Masserot, A, Massinger, T. J, Masso-Reid, M, Mastrogiovanni, S, Matas, A, Matichard, F, Matone, L, Mavalvala, N, Mazumder, N, Mccann, J. J, Mccarthy, R, Mcclelland, D. E, Mccormick, S, Mcculler, L, Mcguire, S. C, Mciver, J, Mcmanus, D. J, Mcrae, T, Mcwilliams, S. T, Meacher, D, Meadors, G. D, Mehmet, M, Mehta, A. K, Meidam, J, Melatos, A, Mendell, G, Mercer, R. A, Mereni, L, Merilh, E. L, Merzougui, M, Meshkov, S, Messenger, C, Messick, C, Metzdorff, R, Meyers, P. M, Miao, H, Michel, C, Middleton, H, Mikhailov, E. E, Milano, L, Miller, A. L, Miller, A, Millhouse, M, Mills, J. C, Milovich-Goff, M. C, Minazzoli, O, Minenkov, Y, Mishkin, A, Mishra, C, Mistry, T, Mitra, S, Mitrofanov, V. P, Mitselmakher, G, Mittleman, R, Mo, G, Moffa, D, Mogushi, K, Mohapatra, S. R. P, Montani, M, Moore, C. J, Moraru, D, Moreno, G, Morisaki, S, Mours, B, Mow-Lowry, C. M, Mukherjee, Arunava and Mukherjee, Mukherjee, S, Mukund, N, Mullavey, A, Munch, J, Muniz, E. A, Muratore, M, Murray, P. G, Nagar, A, Nardecchia, I and Naticchioni, L, Nayak, R. K, Neilson, J, Nelemans, G, Nelson, T. J. N, Nery, M, Neunzert, A, K. Y, Ng, Ng, S, Nguyen, P, Nichols, D, Nissanke, S, Nocera, F, North, C, Nuttall, L. K, Obergaulinger, M, Oberling, J, O'Brien, B. D, O'Dea, G. D, O'Gin, G. H, J. J, Oh, S. H, Oh, Ohme, F, Ohta, H, Okada, M. A, Oliver, M, Oppermann, P, Oram, Richard J, O'Reilly, B, Ormiston, R. G, Ortega, L. F, O'Shaughnessy, R, Ossokine, S, Ottaway, D. J, Overmier, H, Owen, B. J, Pace, A. E, Pagano, G, Page, M. A, Pai, A, Pai, S. A, Palamos, J. R, Palashov, O, Palomba, C, Pal-Singh, A, Pan, Huang-Wei and Pang, Pang, P. T. H, Pankow, C, Pannarale, F, Pant, B. C, Paoletti, F, Paoli, A, Parida, A, Parker, W, Pascucci, D, Pasqualetti, A, Passaquieti, R, Passuello, D, Patil, M, Patricelli, B, Pearlstone, B. L, Pedersen, C, Pedraza, M, Pedurand, R, Pele, A, Penn, S, Perez, C. J, Perreca, A, Pfeiffer, H. P, Phelps, M, Phukon, K. S, Piccinni, O. J, Pichot, M, Piergiovanni, F, Pillant, G, Pinard, L, Pirello, M, Pitkin, M, Poggiani, R, Pong, D. Y. T, Ponrathnam, S, Popolizio, P, Porter, E. K, Powell, J, Prajapati, A. K, Prasad, J, Prasai, K, Prasanna, R, Pratten, G, Prestegard, T, Privitera, S, Prodi, G. A, Prokhorov, L. G, Puncken, O, Punturo, M, Puppo, P, Prrer, M, Qi, H, Quetschke, V and Quinonez, P. J., Quintero, E. A, Quitzow-James, R, Raab, F. J, Radkins, H, Radulescu, N, Raffai, P, Raja, S, Rajan, C, Rajbhandari, B, Rakhmanov, M, Ramirez, K. E, Ramos-Buades, A, Rana, Javed and Rao, Rapagnani, P, Raymond, V and Razzano, Read, J, Regimbau, T, Rei, L, Reid, S, Reitze, D. H, Ren, W, Ricci, F, Richardson, C. J, Richardson, J. W, Ricker, P. M, Riles, K, Rizzo, M, Robertson, N. A, Robie, R, Robinet, F, Rocchi, A, Rolland, L, Rollins, J. G, Roma, V. J, Romanelli, M, Romano, R, Romel, C. L, Romie, J. H, Rose, K, Rosinska, D, Rosofsky, S. G, Ross, M. P, Rowan, S, Ruediger, A, Ruggi, P, Rutins, G, Ryan, K, Sachdev, S, Sadecki, T, Sakellariadou, M, Salconi, L, Saleem, M, Samajdar, A, Sammut, L, Sanchez, E. J, Sanchez, L. E, Sanchis-Gual, N, Sandberg, V and Sanders, J. R., Santiago, K. A, Sarin, N, Sassolas, B, Saulson, P. R, Sauter, O, Savage, R. L, Schale, P, Scheel, M, Scheuer, J, Schmidt, P, Schnabel, R, Schofield, R. M. S, Schoenbeck, A, Schreiber, E, Schulte, B. W, Schutz, B. F, Schwalbe, S. G, Scott, J, Scott, S. M, Seidel, E, Sellers, D, Sengupta, A. S, Sennett, N, Sentenac, D, Sequino, V and Sergeev, Setyawati, Y, Shaddock, D. A, Shaffer, T, Shahriar, M. S, Shaner, M. B, Shao, L, Sharma, P, Shawhan, P, Shen, H, Shink, R, Shoemaker, D. H, Shoemaker, D. M, Shyamsundar, S, Siellez, K, Sieniawska, M, Sigg, D, Silva, A. D, Singer, L. P, Singh, N, Singhal, A, Sintes, A. M, Sitmukhambetov, S, Skliris, V and Slagmolen, B. J. J., Slaven-Blair, T. J, Smith, J. R, Smith, R. J. E, Somala, S, Son, E. J, Sorazu, B, Sorrentino, F, Souradeep, T, Sowell, E, Spencer, A. P, Srivastava, A. K, Srivastava, V and Staats, Stachie, C, Standke, M, Steer, D. A, Steinke, M, Steinlechner, J, Steinlechner, S, Steinmeyer, D, Stevenson, S. P, Stocks, D, Stone, R, Stops, D. J, Strain, K. A, Stratta, G, Strigin, S. E, Strunk, A, Sturani, R, Stuver, A. L, Sudhir, V and Summerscales, T. Z., Sun, L, Sunil, S, Suresh, J, Sutton, P. J, Swinkels, B. L, Szczepanczyk, M. J, Tacca, M, Tait, S. C, Talbot, C, Talukder, D, Tanner, D. B, Tapai, M, Taracchini, A, Tasson, J. D, Taylor, R, Thies, F, Thomas, M, Thomas, P, Thondapu, S. R, Thorne, K. A, Thrane, E, Tiwari, Shubhanshu and Tiwari, Srishti and Tiwari, V and Toland, Tonelli, M, Tornasi, Z, Torres-Forn, A, Torrie, Tyr, D, Travasso, F, Traylor, G, Tringali, M. C, Trovato, A, Trozzo, L, Trudeau, R, Tsang, K. W, Tse, M, Tso, R, Tsukada, L, Tsuna, D, Tuyenbayev, D, Ueno, K, Ugolini, D, Unnikrishnan, C. S, Urban, A. L, Usman, S. A, Vahlbruch, H, Vajente, G, Valdes, G, van Bakel, N, van Beuzekom, M, van den Brand, J. F. J, Van Den Broeck, C, Vander-Hyde, D. C, Van, Heijningen, van der Schaaf, L, van Veggel, A. A, Vardaro, M, Varma, V, Vass, S, Vasuth, M, Vecchio, A, Vedovato, G, Veitch, J, Veitch, P. J, Venkateswara, K, Venugopalan, G, Verkindt, D, Vetrano, F, Vicere, A, Viets, A. D, Vine, D. J, Vinet, J-Y and Vitale, Vo, T, Vocca, H, Vorvick, C, Vyatchanin, S. P, Wade, A. R, Wade, L. E, Wade, M, Walet, R, Walker, M, Wallace, L, Walsh, S, Wang, G, Wang, H, Wang, J. Z, Wang, W. H, Wang, Y. F, Ward, R. L, Warden, Z. A, Warner, J, Was, M, Watchi, J, Weaver, B, Wei, L-W and Weinert, Weinstein, A. J, Weiss, R, Wellmann, F, Wen, L, Wessel, E. K, Wessels, P, Westhouse, J. W, Wette, K, Whelan, J. T, Whiting, B. F, Whittle, C, Wilken, D. M, Williams, D, Williamson, A. R, Willis, J. L, Willke, B, Wimmer, M. H, Winkler, W, Wipf, C. C, Wittel, H, Woan, G, Woehler, J, Wofford, J. K, Worden, J, Wright, J. L, D. S, Wu, Wysocki, D. M, Xiao, L, Yamamoto, H, Yancey, C. C, Yang, L, Yap, M. J, Yazback, M, Yeeles, D. W, Hang and Yu, Haocun and Yuen, S. H. R., Yvert, M, Zadrozny, A. K, Zanolin, M, Zelenova, T, Zendri, J-P and Zevin, Zhang, J, Zhang, L, Zhang, T, Zhao, C, Zhou, M, Zhou, Z, Zhu, X. J, Zucker, M. E, Zweizig, J., Laboratoire des matériaux avancés (LMA), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut des Fonctions Optiques pour les Technologies de l'informatiON (Institut FOTON), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-École Nationale Supérieure des Sciences Appliquées et de Technologie (ENSSAT)-Centre National de la Recherche Scientifique (CNRS)-Université Bretagne Loire (UBL)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), Laboratoire Kastler Brossel (LKB [Collège de France]), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Collège de France (CdF)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon, ESPCI ParisTech, Institut des Hautes Etudes Scientifiques (IHES), IHES, LIGO Scientific, Virgo, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire 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Babak, S, Bacon, P, Badaracco, F, Bader, Mkm, Bae, S, Baker, Pt, Baldaccini, F, Ballardin, G, Ballmer, Sw, Banagiri, S, Barayoga, Jc, Barclay, Se, Barish, Bc, Barker, D, Barkett, K, Barnum, S, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Bartos, I, Bassiri, R, Basti, A, Bawaj, M, Bayley, Jc, Bazzan, M, Becsy, B, Bejger, M, Belahcene, I, Bell, A, Beniwal, D, Berger, Bk, Bergmann, G, Bernuzzi, S, Bero, Jj, Berry, Cpl, Bersanetti, D, Bertolini, A, Betzwieser, J, Bhandare, R, Bidler, J, Bilenko, Ia, Bilgili, Sa, Billingsley, G, Birch, J, Birney, R, Birnholtz, O, Biscans, S, Biscoveanu, S, Bisht, A, Bitossi, M, Bizouard, Ma, Blackburn, Jk, Blair, Cd, Blair, Dg, Blair, Rm, Bloemen, S, Bode, N, Boer, M, Boetzel, Y, Bogaert, G, Bondu, F, Bonilla, E, Bonnand, R, Booker, P, Boom, Ba, Booth, Cd, Bork, R, Boschi, V, Bose, S, Bossie, K, Bossilkov, V, Bosveld, J, Bouffanais, Y, Bozzi, A, Bradaschia, C, Brady, Pr, Bramley, A, Branchesi, M, Brau, Je, Briant, T, Briggs, Jh, 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Dooley, Kl, Doravari, S, Dorrington, I, Downes, Tp, Drago, M, Driggers, Jc, Du, Z, Ducoin, Jg, Dupej, P, Dwyer, Se, Easter, Pj, Edo, Tb, Edwards, Mc, Effler, A, Ehrens, P, Eichholz, J, Eikenberry, S, Eisenmann, M, Eisenstein, Ra, Essick, Rc, Estelles, H, Estevez, D, Etienne, Zb, Etzel, T, Evans, M, Evans, Tm, Fafone, V, Fair, H, Fairhurst, S, Fan, X, Farinon, S, Farr, B, Farr, Wm, Fauchon-Jones, Ej, Favata, M, Fays, M, Fazio, M, Fee, C, Feicht, J, Fejer, Mm, Feng, F, Fernandez-Galiana, A, Ferrante, I, Ferreira, Ec, Ferreira, Ta, Ferrini, F, Fidecaro, F, Fiori, I, Fiorucci, D, Fishbach, M, Fisher, Rp, Fishner, Jm, Fitz-Axen, M, Flaminio, R, Fletcher, M, Flynn, E, Fong, H, Font, Ja, Forsyth, Pwf, Fournier, Jd, Frasca, S, Frasconi, F, Frei, Z, Freise, A, Frey, R, Frey, V, Fritschel, P, Frolov, Vv, Fulda, P, Fyffe, M, Gabbard, Ha, Gadre, Bu, Gaebel, Sm, Gair, Jr, Gammaitoni, L, Ganija, Mr, Gaonkar, Sg, Garcia, A, Garcia-Quiros, C, Garufi, F, Gateley, B, Gaudio, S, Gaur, G, Gayathri, V, 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Hofman, D, Holgado, Am, Holland, Na, Holt, K, Holz, De, Hopkins, P, Horst, C, Hough, J, Howell, Ej, Hoy, Cg, Hreibi, A, Huerta, Ea, Huet, D, Hughey, B, Hulko, M, Husa, S, Huttner, Sh, Huynh-Dinh, T, Idzkowski, B, Iess, A, Ingram, C, Inta, R, Intini, G, Irwin, B, Isa, Hn, Isac, Jm, Isi, M, Iyer, Br, Izumi, K, Jacqmin, T, Jadhav, Sj, Jani, K, Janthalur, Nn, Jaranowski, P, Jenkins, Ac, Jiang, J, Johnson, D, Jones, Aw, Jones, Di, Jones, R, Jonker, Rjg, Ju, L, Junker, J, Kalaghatgi, Cv, Kalogera, V, Kamai, B, Kandhasamy, S, Kang, G, Kanner, Jb, Kapadia, Sj, Karki, S, Karvinen, K, Kashyap, R, Kasprzack, M, Katsanevas, S, Katsavounidis, E, Katzman, W, Kaufer, S, Kawabe, K, Keerthana, Nv, Kefelian, F, Keitel, D, Kennedy, R, Key, J, Khalili, Fy, Khan, H, Khan, I, Khan, S, Khan, Z, Khazanov, Ea, Khursheed, M, Kijbunchoo, N, Kim, C, Kim, Jc, Kim, K, Kim, W, Kim, Ym, Kimball, C, King, Ej, King, Pj, Kinley-Hanlon, M, Kirchhoff, R, Kissel, J, Kleybolte, L, Klika, Jh, Klimenko, S, Knowles, Td, Koch, P, Koehlenbeck, Sm, Koekoek, G, Koley, S, Kondrashov, V, Kontos, A, Koper, N, Korobko, M, Korth, Wz, Kowalska, I, Kozak, Db, Kringel, V, Krishnendu, N, Krlak, A, Kuehn, G, Kumar, A, Kumar, P, Kumar, R, Kumar, S, Kuo, L, Kutynia, A, Kwang, S, Lackey, Bd, Lai, Kh, Lam, Tl, Landry, M, Lane, Bb, Lang, Rn, Lange, J, Lantz, B, Lanza, Rk, Lartaux-Vollard, A, Lasky, Pd, Laxen, M, Lazzarini, A, Lazzaro, C, Leaci, P, Leavey, S, Lecoeuche, Yk, Lee, Ch, Lee, Hk, Lee, Hm, Lee, Hw, Lee, J, Lee, K, Lehmann, J, Lenon, A, Leroy, N, Letendre, N, Levin, Y, Li, J, Li, Kjl, Li, Tgf, Li, X, Lin, F, Linde, F, Linker, Sd, Littenberg, Tb, Liu, J, Liu, X, Lo, Rkl, Lockerbie, Na, London, Lt, Longo, A, Lorenzini, M, Loriette, V, Lormand, M, Losurdo, G, Lough, Jd, Lousto, Co, Lovelace, G, Lower, Me, Luck, H, Lumaca, D, Lundgren, Ap, Lynch, R, Ma, Y, Macas, R, Macfoy, S, Macinnis, M, Macleod, Dm, Macquet, A, Magana-Sandoval, F, Zertuche, Lm, Magee, Rm, Majorana, E, Maksimovic, I, Malik, A, Man, N, Mandic, V, 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Steinlechner, J, Steinlechner, S, Steinmeyer, D, Stevenson, Sp, Stocks, D, Stone, R, Stops, Dj, Strain, Ka, Stratta, G, Strigin, Se, Strunk, A, Sturani, R, Stuver, Al, Sudhir, V, Summerscales, Tz, Sun, L, Sunil, S, Suresh, J, Sutton, Pj, Swinkels, Bl, Szczepanczyk, Mj, Tacca, M, Tait, Sc, Talbot, C, Talukder, D, Tanner, Db, Tapai, M, Taracchini, A, Tasson, Jd, Taylor, R, Thies, F, Thomas, M, Thomas, P, Thondapu, Sr, Thorne, Ka, Thrane, E, Tiwari, S, Tiwari, V, Toland, K, Tonelli, M, Tornasi, Z, Torres-Forn, A, Torrie, Ci, Tyr, D, Travasso, F, Traylor, G, Tringali, Mc, Trovato, A, Trozzo, L, Trudeau, R, Tsang, Kw, Tse, M, Tso, R, Tsukada, L, Tsuna, D, Tuyenbayev, D, Ueno, K, Ugolini, D, Unnikrishnan, C, Urban, Al, Usman, Sa, Vahlbruch, H, Vajente, G, Valdes, G, van Bakel, N, van Beuzekom, M, van den Brand, Jfj, Van Den Broeck, C, Vander-Hyde, Dc, van Heijningen, Jv, van der Schaaf, L, van Veggel, Aa, Vardaro, M, Varma, V, Vass, S, Vasuth, M, Vecchio, A, Vedovato, G, Veitch, J, Veitch, 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Abbott, B. P., Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, G., Allocca, A., Aloy, M. A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arene, M., Arnaud, N., Ascenzi, S., Ashton, G., Aston, S. M., Astone, P., Aubin, F., Aufmuth, P., Aultoneal, K., Austin, C., Avendano, V., Avila-Alvarez, A., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Bazzan, M., Becsy, B., Bejger, M., Belahcene, I., Bell, A. 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C., Dietrich, T., Di Fiore, L., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Ding, B., Di Pace, S., Di Palma, I., Di Renzo, F., Dmitriev, A., Doctor, Z., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Downes, T. P., Drago, M., Driggers, J. C., Du, Z., Ducoin, J. -G., Dupej, P., Dwyer, S. E., Easter, P. J., Edo, T. B., Edwards, M. C., Effler, A., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenmann, M., Eisenstein, R. A., Essick, R. C., Estelles, H., Estevez, D., Etienne, Z. B., Etzel, T., Evans, M., Evans, T. M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fazio, M., Fee, C., Feicht, J., Fejer, M. M., Feng, F., Fernandez-Galiana, A., Ferrante, I., Ferreira, E. C., Ferreira, T. A., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fishbach, M., Fisher, R. P., Fishner, J. M., Fitz-Axen, M., Flaminio, R., Fletcher, M., Flynn, E., Fong, H., Font, J. A., Forsyth, P. W. 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K., Gustafson, R., Haegel, L., Halim, O., Hall, B. R., Hall, E. D., Hamilton, E. Z., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannuksela, O. A., Hanson, J., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Haster, C. -J., Haughian, K., Hayes, F. J., Healy, J., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Vivanco, F. H., Heurs, M., Hild, S., Hinderer, T., Hoak, D., Hochheim, S., Hofman, D., Holgado, A. M., Holland, N. A., Holt, K., Holz, D. E., Hopkins, P., Horst, C., Hough, J., Howell, E. J., Hoy, C. G., Hreibi, A., Huerta, E. A., Huet, D., Hughey, B., Hulko, M., Husa, S., Huttner, S. H., Huynh-Dinh, T., Idzkowski, B., Iess, A., Ingram, C., Inta, R., Intini, G., Irwin, B., Isa, H. N., Isac, J. -M., Isi, M., Iyer, B. R., Izumi, K., Jacqmin, T., Jadhav, S. J., Jani, K., Janthalur, N. N., Jaranowski, P., Jenkins, A. C., Jiang, J., Johnson, D. S., Jones, A. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Junker, J., Kalaghatgi, C. V., Kalogera, V., Kamai, B., Kandhasamy, S., Kang, G., Kanner, J. B., Kapadia, S. J., Karki, S., Karvinen, K. S., Kashyap, R., Kasprzack, M., Katsanevas, S., Katsavounidis, E., Katzman, W., Kaufer, S., Kawabe, K., Keerthana, N. V., Kefelian, F., Keitel, D., Kennedy, R., Key, J. S., Khalili, F. Y., Khan, H., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Khursheed, M., Kijbunchoo, N., Kim, C., Kim, J. C., Kim, K., Kim, W., Kim, W. S., Kim, Y. -M., Kimball, C., King, E. J., King, P. J., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Kleybolte, L., Klika, J. H., Klimenko, S., Knowles, T. D., Koch, P., Koehlenbeck, S. M., Koekoek, G., Koley, S., Kondrashov, V., Kontos, A., Koper, N., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Kringel, V., Krishnendu, N., Krolak, A., Kuehn, G., Kumar, A., Kumar, P., Kumar, R., Kumar, S., Kuo, L., Kutynia, A., Kwang, S., Lackey, B. D., Lai, K. H., Lam, T. L., Landry, M., Lane, B. B., Lang, R. N., Lange, J., Lantz, B., Lanza, R. K., Lartaux-Vollard, A., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lecoeuche, Y. K., Lee, C. H., Lee, H. K., Lee, H. M., Lee, H. W., Lee, J., Lee, K., Lehmann, J., Lenon, A., Leroy, N., Letendre, N., Levin, Y., Li, J., Li, K. J. L., Li, T. G. F., Li, X., Lin, F., Linde, F., Linker, S. D., Littenberg, T. B., Liu, J., Liu, X., Lo, R. K. L., Lockerbie, N. A., London, L. T., Longo, A., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lousto, C. O., Lovelace, G., Lower, M. E., Luck, H., Lumaca, D., Lundgren, A. P., Lynch, R., Ma, Y., Macas, R., Macfoy, S., Macinnis, M., Macleod, D. M., Macquet, A., Magana-Sandoval, F., Zertuche, L. M., Magee, R. M., Majorana, E., Maksimovic, I., Malik, A., Man, N., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Marka, S., Marka, Z., Markakis, C., Markosyan, A. S., Markowitz, A., Maros, E., Marquina, A., Marsat, S., Martelli, F., Martin, I. W., Martin, R. M., Martynov, D. V., Mason, K., Massera, E., Masserot, A., Massinger, T. J., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., Mccann, J. J., Mccarthy, R., Mcclelland, D. E., Mccormick, S., Mcculler, L., Mcguire, S. C., Mciver, J., Mcmanus, D. J., Mcrae, T., Mcwilliams, S. T., Meacher, D., Meadors, G. D., Mehmet, M., Mehta, A. K., Meidam, J., Melatos, A., Mendell, G., Mercer, R. A., Mereni, L., Merilh, E. L., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Metzdorff, R., Meyers, P. M., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, L., Miller, A. L., Miller, A., Millhouse, M., Mills, J. C., Milovich-Goff, M. C., Minazzoli, O., Minenkov, Y., Mishkin, A., Mishra, C., Mistry, T., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Mo, G., Moffa, D., Mogushi, K., Mohapatra, S. R. P., Montani, M., Moore, C. J., Moraru, D., Moreno, G., Morisaki, S., Mours, B., Mow-Lowry, C. M., Mukherjee, A., Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Muniz, E. A., Muratore, M., Murray, P. G., Nagar, A., Nardecchia, I., Naticchioni, L., Nayak, R. K., Neilson, J., Nelemans, G., Nelson, T. J. N., Nery, M., Neunzert, A., Ng, K. Y., Ng, S., Nguyen, P., Nichols, D., Nissanke, S., Nocera, F., North, C., Nuttall, L. K., Obergaulinger, M., Oberling, J., O'Brien, B. D., O'Dea, G. D., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Ohta, H., Okada, M. A., Oliver, M., Oppermann, P., Oram, R. J., O'Reilly, B., Ormiston, R. G., Ortega, L. F., O'Shaughnessy, R., Ossokine, S., Ottaway, D. J., Overmier, H., Owen, B. J., Pace, A. E., Pagano, G., Page, M. A., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pal-Singh, A., Pan, H. -W., Pang, B., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Parida, A., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patil, M., Patricelli, B., Pearlstone, B. L., Pedersen, C., Pedraza, M., Pedurand, R., Pele, A., Penn, S., Perez, C. J., Perreca, A., Pfeiffer, H. P., Phelps, M., Phukon, K. S., Piccinni, O. J., Pichot, M., Piergiovanni, F., Pillant, G., Pinard, L., Pirello, M., Pitkin, M., Poggiani, R., Pong, D. Y. T., Ponrathnam, S., Popolizio, P., Porter, E. K., Powell, J., Prajapati, A. K., Prasad, J., Prasai, K., Prasanna, R., Pratten, G., Prestegard, T., Privitera, S., Prodi, G. A., Prokhorov, L. G., Puncken, O., Punturo, M., Puppo, P., Purrer, M., Qi, H., Quetschke, V., Quinonez, P. J., Quintero, E. A., Quitzow-James, R., Raab, F. J., Radkins, H., Radulescu, N., Raffai, P., Raja, S., Rajan, C., Rajbhandari, B., Rakhmanov, M., Ramirez, K. E., Ramos-Buades, A., Rana, J., Rao, K., Rapagnani, P., Raymond, V., Razzano, M., Read, J., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Ren, W., Ricci, F., Richardson, C. J., Richardson, J. W., Ricker, P. M., Riles, K., Rizzo, M., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romanelli, M., Romano, R., Romel, C. L., Romie, J. H., Rose, K., Rosinska, D., Rosofsky, S. G., Ross, M. P., Rowan, S., Rudiger, A., Ruggi, P., Rutins, G., Ryan, K., Sachdev, S., Sadecki, T., Sakellariadou, M., Salconi, L., Saleem, M., Samajdar, A., Sammut, L., Sanchez, E. J., Sanchez, L. E., Sanchis-Gual, N., Sandberg, V., Sanders, J. R., Santiago, K. A., Sarin, N., Sassolas, B., Saulson, P. R., Sauter, O., Savage, R. L., Schale, P., Scheel, M., Scheuer, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schonbeck, A., Schreiber, E., Schulte, B. W., Schutz, B. F., Schwalbe, S. G., Scott, J., Scott, S. M., Seidel, E., Sellers, D., Sengupta, A. S., Sennett, N., Sentenac, D., Sequino, V., Sergeev, A., Setyawati, Y., Shaddock, D. A., Shaffer, T., Shahriar, M. S., Shaner, M. B., Shao, L., Sharma, P., Shawhan, P., Shen, H., Shink, R., Shoemaker, D. H., Shoemaker, D. M., Shyamsundar, S., Siellez, K., Sieniawska, M., Sigg, D., Silva, A. D., Singer, L. P., Singh, N., Singhal, A., Sintes, A. M., Sitmukhambetov, S., Skliris, V., Slagmolen, B. J. J., Slaven-Blair, T. J., Smith, J. R., Smith, R. J. E., Somala, S., Son, E. J., Sorazu, B., Sorrentino, F., Souradeep, T., Sowell, E., Spencer, A. P., Srivastava, A. K., Srivastava, V., Staats, K., Stachie, C., Standke, M., Steer, D. A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stevenson, S. P., Stocks, D., Stone, R., Stops, D. J., Strain, K. A., Stratta, G., Strigin, S. E., Strunk, A., Sturani, R., Stuver, A. L., Sudhir, V., Summerscales, T. Z., Sun, L., Sunil, S., Suresh, J., Sutton, P. J., Swinkels, B. L., Szczepanczyk, M. J., Tacca, M., Tait, S. C., Talbot, C., Talukder, D., Tanner, D. B., Tapai, M., Taracchini, A., Tasson, J. D., Taylor, R., Thies, F., Thomas, M., Thomas, P., Thondapu, S. R., Thorne, K. A., Thrane, E., Tiwari, S., Tiwari, V., Toland, K., Tonelli, M., Tornasi, Z., Torres-Forne, A., Torrie, C. I., Toyra, D., Travasso, F., Traylor, G., Tringali, M. C., Trovato, A., Trozzo, L., Trudeau, R., Tsang, K. W., Tse, M., Tso, R., Tsukada, L., Tsuna, D., Tuyenbayev, D., Ueno, K., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., Van Bakel, N., Van Beuzekom, M., Van Den Brand, J. F. J., Van Den Broeck, C., Vander-Hyde, D. C., Van Heijningen, J. V., Van Der Schaaf, L., Van Veggel, A. A., Vardaro, M., Varma, V., Vass, S., Vasuth, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Venugopalan, G., Verkindt, D., Vetrano, F., Vicere, A., Viets, A. D., Vine, D. J., Vinet, J. -Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walet, R., Walker, M., Wallace, L., Walsh, S., Wang, G., Wang, H., Wang, J. Z., Wang, W. H., Wang, Y. F., Ward, R. L., Warden, Z. A., Warner, J., Was, M., Watchi, J., Weaver, B., Wei, L. -W., Weinert, M., Weinstein, A. J., Weiss, R., Wellmann, F., Wen, L., Wessel, E. K., Wessels, P., Westhouse, J. W., Wette, K., Whelan, J. T., Whiting, B. F., Whittle, C., Wilken, D. M., Williams, D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M. H., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Woehler, J., Wofford, J. K., Worden, J., Wright, J. L., Wu, D. S., Wysocki, D. M., Xiao, L., Yamamoto, H., Yancey, C. C., Yang, L., Yap, M. J., Yazback, M., Yeeles, D. W., Yu, H., Yuen, S. H. R., Yvert, M., Zadrozny, A. K., Zanolin, M., Zelenova, T., Zendri, J. -P., Zevin, M., Zhang, J., Zhang, L., Zhang, T., Zhao, C., Zhou, M., Zhou, Z., Zhu, X. J., Zucker, M. E., Zweizig, J., The LIGO Scientific Collaboration, The Virgo Collaboration, Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-École Nationale Supérieure des Sciences Appliquées et de Technologie (ENSSAT)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF (institution))-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut des Hautes Études Scientifiques (IHES), (Astro)-Particles Physics, Abbott, B, Abbott, T, Adhikari, R, Adya, V, Aguiar, O, Aloy, M, Altin, P, Anderson, S, Anderson, W, Angelova, S, Araya, M, Arène, M, Aston, S, Bader, M, Baker, P, Ballmer, S, Barayoga, J, Barclay, S, Barish, B, Bayley, J, Bécsy, B, Berger, B, Bero, J, Berry, C, Bilenko, I, Bilgili, S, Bizouard, M, Blackburn, J, Blair, C, Blair, D, Blair, R, Boom, B, Booth, C, Brady, P, Brau, J, Briggs, J, Brooks, A, Brown, D, Bulten, H, Byer, R, Bustillo, J, Callister, T, Camp, J, Campbell, W, Cannon, K, Carney, M, Diaz, J, Cavaglià, M, Cerdá-Durán, P, Chamberlin, S, Chase, E, Cheeseboro, B, Chen, H, Cheng, H, Cheong, C, Chia, H, Chung, K, Ciobanu, A, Clark, J, Cohadon, P, Collette, C, Cominsky, L, Cooper, S, Corbitt, T, Cordero-Carrión, I, Corley, K, Costa, C, Coughlin, M, Coughlin, S, Coulon, J, Countryman, S, Covas, P, Cowan, E, Coward, D, Cowart, M, Coyne, D, Creighton, J, Creighton, T, Crowder, S, Cullen, T, Canton, T, Dálya, G, Danilishin, S, D’Antonio, S, Da Silva Costa, C, Datrier, L, Daw, E, Deléglise, S, Demarchi, L, Díaz, M, Dooley, K, Downes, T, Driggers, J, Ducoin, J, Dwyer, S, Easter, P, Edo, T, Edwards, M, Eisenstein, R, Essick, R, Etienne, Z, Evans, T, Farr, W, Fauchon-Jones, E, Fejer, M, Ferreira, E, Ferreira, T, Fisher, R, Fishner, J, Font, J, Forsyth, P, Fournier, J, Frolov, V, Gabbard, H, Gadre, B, Gaebel, S, Gair, J, Ganija, M, Gaonkar, S, García-Quirós, C, Giaime, J, Giardina, K, González, G, Gonzalez Castro, J, Gorodetsky, M, Gossan, S, Green, A, Gretarsson, E, Guidi, G, Gulati, H, Gupta, M, Gustafson, E, Hall, B, Hall, E, Hamilton, E, Hanke, M, Hannuksela, O, Harry, G, Harry, I, Haster, C, Hayes, F, Heintze, M, Heptonstall, A, Vivanco, F, Holgado, A, Holland, N, Holz, D, Howell, E, Hoy, C, Huerta, E, Huttner, S, Isa, H, Isac, J, Iyer, B, Jadhav, S, Janthalur, N, Jenkins, A, Jones, A, Jones, D, Jonker, R, Kalaghatgi, C, Kanner, J, Kapadia, S, Keerthana, N, Kéfélian, F, Khalili, F, Khazanov, E, Kim, J, Kim, Y, King, E, King, P, Klika, J, Knowles, T, Koehlenbeck, S, Korth, W, Kozak, D, Królak, A, Lackey, B, Lai, K, Lam, T, Lane, B, Lang, R, Lanza, R, Lasky, P, Lecoeuche, Y, Lee, C, Lee, H, Li, K, Li, T, Linker, S, Littenberg, T, Lo, R, Lockerbie, N, London, L, Lough, J, Lousto, C, Lower, M, Lück, H, Lundgren, A, Macleod, D, Magaña-Sandoval, F, Zertuche, L, Magee, R, Mansell, G, Márka, S, Márka, Z, Martin, I, Martin, R, Martynov, D, Massinger, T, Mccann, J, Mcclelland, D, Mcguire, S, Mcmanus, D, Mcwilliams, S, Meadors, G, Mehta, A, Mercer, R, Merilh, E, Meyers, P, Mikhailov, E, Mills, J, Milovich-Goff, M, Mitrofanov, V, Mohapatra, S, Moore, C, Mow-Lowry, C, Muñiz, E, Murray, P, Nayak, R, Nelson, T, Ng, K, Nuttall, L, O’Brien, B, O’Dea, G, Ogin, G, Oh, J, Oh, S, Okada, M, Oram, R, O’Reilly, B, Ormiston, R, Ortega, L, O’Shaughnessy, R, Ottaway, D, Owen, B, Pace, A, Page, M, Pai, S, Palamos, J, Pan, H, Pang, P, Pant, B, Pearlstone, B, Perez, C, Pfeiffer, H, Piccinni, O, Pong, D, Porter, E, Prajapati, A, Prodi, G, Prokhorov, L, Pürrer, M, Quinonez, P, Quintero, E, Raab, F, Ramirez, K, Reitze, D, Richardson, C, Richardson, J, Ricker, P, Robertson, N, Rollins, J, Roma, V, Romel, C, Romie, J, Rosińska, D, Rosofsky, S, Ross, M, Rüdiger, A, Sanchez, E, Sanchez, L, Sanders, J, Santiago, K, Saulson, P, Savage, R, Schofield, R, Schönbeck, A, Schulte, B, Schutz, B, Schwalbe, S, Scott, S, Shaddock, D, Shaner, M, Shoemaker, D, Silva, A, Singer, L, Sintes, A, Slagmolen, B, Slaven-Blair, T, Smith, J, Smith, R, Son, E, Spencer, A, Srivastava, A, Steer, D, Stevenson, S, Stops, D, Strain, K, Strigin, S, Stuver, A, Summerscales, T, Sutton, P, Swinkels, B, Szczepańczyk, M, Tait, S, Tanner, D, Tápai, M, Tasson, J, Thondapu, S, Thorne, K, Torres-Forné, A, Torrie, C, Töyrä, D, Tringali, M, Tsang, K, Urban, A, Usman, S, van den Brand, J, Vander-Hyde, D, van Heijningen, J, van Veggel, A, Vasúth, M, Veitch, P, Viceré, A, Viets, A, Vine, D, Vinet, J, Vyatchanin, S, Wade, A, Wade, L, Wang, J, Wang, W, Wang, Y, Ward, R, Warden, Z, Wei, L, Weinstein, A, Wessel, E, Weßels, P, Westhouse, J, Whelan, J, Whiting, B, Wilken, D, Williamson, A, Willis, J, Wimmer, M, Wipf, C, Wofford, J, Wright, J, Wysocki, D, Yancey, C, Yap, M, Yeeles, D, Yuen, S, Zadrożny, A, Zendri, J, Zhu, X, and Zucker, M
- Subjects
noise ,010504 meteorology & atmospheric sciences ,Astronomy ,FOS: Physical sciences ,Astrophysics ,gravitational waves ,stars: magnetars ,Astronomy and Astrophysics ,Space and Planetary Science ,Astronomy & Astrophysics ,Magnetar ,01 natural sciences ,0103 physical sciences ,magnetars [stars] ,Sensitivity (control systems) ,gravitational radiation: energy ,SDG 7 - Affordable and Clean Energy ,LIGO ,010303 astronomy & astrophysics ,gravitational wave ,STFC ,QC ,0105 earth and related environmental sciences ,QB ,Physics ,astro-ph.HE ,Settore FIS/01 ,High Energy Astrophysical Phenomena (astro-ph.HE) ,Science & Technology ,Gravitational wave ,X-RAY OSCILLATIONS ,RCUK ,White noise ,magnetar ,sensitivity ,Orientation (vector space) ,Physics and Astronomy ,efficiency ,DISCOVERY ,Physical Sciences ,Astrophysics - High Energy Astrophysical Phenomena ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,burst ,Energy (signal processing) ,Dimensionless quantity - Abstract
We present the results of a search for short- and intermediate-duration gravitational-wave signals from four magnetar bursts in Advanced LIGO’s second observing run. We find no evidence of a signal and set upper bounds on the root sum squared of the total dimensionless strain (h rss) from incoming intermediate-duration gravitational waves ranging from 1.1 × 10-22 at 150 Hz to 4.4 × 10-22 at 1550 Hz at 50% detection efficiency. From the known distance to the magnetar SGR 1806-20 (8.7 kpc), we can place upper bounds on the isotropic gravitational-wave energy of 3.4 × 1044 erg at 150 Hz assuming optimal orientation. This represents an improvement of about a factor of 10 in strain sensitivity from the previous search for such signals, conducted during initial LIGO’s sixth science run. The short-duration search yielded upper limits of 2.1 × 1044 erg for short white noise bursts, and 2.3 × 1047 erg for 100 ms long ringdowns at 1500 Hz, both at 50% detection efficiency. ispartof: ASTROPHYSICAL JOURNAL vol:874 issue:2 status: published
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- 2019
4. Superthermal Proton and Electron Fluxes in the Plasma Sheet Transition Region and Their Dependence on Solar Wind Parameters
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V. A. Sergeev, Natalia Ganushkina, Vassilis Angelopoulos, V. A. Andreeva, Stepan Dubyagin, Andrei Runov, N. A. Stepanov, and D. A. Sormakov
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Solar wind ,Geophysics ,Materials science ,Proton ,Space and Planetary Science ,Plasma sheet ,Electron ,Atomic physics - Published
- 2021
5. Remote Sensing of Magnetic Reconnection in the Magnetotail Using In Situ Multipoint Observations at the Plasma Sheet Boundary Layer
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V. A. Sergeev, Barbara L. Giles, Justin Holmes, Simon Wellenzohn, S. Apatenkov, Takuma Nakamura, Rumi Nakamura, Elena Grigorenko, Roy B. Torbert, James L. Burch, and A. Varsani
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In situ ,Physics ,Boundary layer ,Geophysics ,Space and Planetary Science ,Remote sensing (archaeology) ,Plasma sheet ,Energy dispersion ,Magnetic reconnection - Published
- 2021
6. Correction to: The ELFIN Mission
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A. Gonzalez, A. Flemming, Eric Grimes, D. Branchevsky, A. Subramanian, D. M. Frederick, K. Hector, D. Hinkley, W. Greer, J. Mao, E. McKinney, A. Tan, A. Norris, A. J. Villegas, E. S. Y. Park, C. Shaffer, M. Cliffe, C. Wong, M. Anderson, R. Krieger, K. Lian, A. V. Artemyev, Ian Fox, B. Hesford, P. Cruce, G. Chao, C. E. Pedersen, J. Artinger, R. Rozario, M. Allen, Robert J. Strangeway, Richard E. Wirz, K. Colton, B. W. Domae, R. Seaton, Wen Li, N. Chung, J. Asher, J. B. Blake, Susmit Jha, M. Chung, A. Palla, D. Leneman, M. Wasden, R. Yap, E. Rye, V. A. Sergeev, D. Depe, A. Gildemeister, Drew Turner, Catherine E. Costello, S. R. Sundin, C. Wilkins, Emmanuel Masongsong, L. Fitzgibbon, A. Gilbert, S. Eldin, C. L. Russell, L. Bingley, R. Caron, G. Y. Zhang, Z. Qu, E. Xie, G. Wing, J. King, Xiao-Jia Zhang, R. Castro, E. Tsai, Jiang Liu, Vassilis Angelopoulos, W. Turner, M. Arreola-Zamora, Andrei Runov, N. Kang, M. Nuesca, S. Yamamoto, J. P. Miller, A. Zarifian, Yuri Shprits, N. Adair, M. R. Capitelli, and M. J. Lawson
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Final version ,Planetary science ,Space and Planetary Science ,Art history ,Astronomy and Astrophysics ,Space (commercial competition) - Abstract
Correction to: Space Sci. Rev. (2020) 216: 103 Affiliation 2 in this article is the wrong affiliation that instead should read: “Institute of Geophysics and Planetary Physics, University of California, Los Angeles, CA, USA” which should be regarded as the final version by the reader.
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- 2020
7. The ELFIN Mission
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V. Angelopoulos, A. Flemming, M. R. Capitelli, C. L. Russell, J. King, Eric Grimes, R. Caron, M. J. Lawson, A. Palla, Susmit Jha, K. Hector, S. R. Sundin, A. Subramanian, Drew Turner, L. Bingley, A. Gilbert, M. Cliffe, Xiao-Jia Zhang, Yuri Shprits, R. Castro, E. Tsai, A. Zarifian, Ian Fox, Richard E. Wirz, Andrei Runov, C. E. Pedersen, A. Tan, C. Wilkins, A. Norris, B. Hesford, E. McKinney, C. Wong, E. Rye, Catherine E. Costello, N. Adair, D. Depe, R. Krieger, R. Rozario, C. Shaffer, Emmanuel Masongsong, J. Mao, J. B. Blake, N. Kang, M. Wasden, K. Colton, Robert J. Strangeway, D. Leneman, M. Allen, Wen Li, B. W. Domae, R. Yap, W. Greer, M. Chung, Anton Artemyev, A. J. Villegas, K. Lian, G. Chao, M. Arreola-Zamora, D. Hinkley, M. Nuesca, S. Yamamoto, J. P. Miller, A. Gildemeister, G. Wing, W. Turner, Jiang Liu, P. Cruce, V. A. Sergeev, A. Gonzalez, D. Branchevsky, N. Chung, J. Asher, M. Anderson, J. Artinger, R. Seaton, L. Fitzgibbon, G. Y. Zhang, Z. Qu, E. Xie, D. M. Frederick, S. Eldin, and E. S. Y. Park
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Physics - Instrumentation and Detectors ,010504 meteorology & atmospheric sciences ,Van Allen radiation belts ,Magnetosphere ,Electron ,Astrophysics ,01 natural sciences ,7. Clean energy ,Physics - Geophysics ,Physics - Space Physics ,Special Communication ,Particle precipitation ,physics.plasm-ph ,physics.ins-det ,010303 astronomy & astrophysics ,Physics ,CubeSat ,Fluxgate magnetometer ,Instrumentation and Detectors (physics.ins-det) ,Orbital period ,physics.geo-ph ,physics.space-ph ,Van Allen radiation belt ,Physics::Space Physics ,symbols ,EMIC ,Ionosphere ,Astronomical and Space Sciences ,FOS: Physical sciences ,Electron precipitation ,Astronomy & Astrophysics ,Energetic particle detector ,symbols.namesake ,0103 physical sciences ,0105 earth and related environmental sciences ,Scattering ,electromagnetic ion cyclotron waves ,Astronomy and Astrophysics ,Auroral ,Physics - Plasma Physics ,Space Physics (physics.space-ph) ,Geophysics (physics.geo-ph) ,Plasma Physics (physics.plasm-ph) ,Space and Planetary Science ,Loss cone ,UCLA ,Pitch angle scattering ,Satellite - Abstract
The Electron Loss and Fields Investigation with a Spatio-Temporal Ambiguity-Resolving option (ELFIN-STAR, or simply: ELFIN) mission comprises two identical 3-Unit (3U) CubeSats on a polar (~93deg inclination), nearly circular, low-Earth (~450 km altitude) orbit. Launched on September 15, 2018, ELFIN is expected to have a >2.5 year lifetime. Its primary science objective is to resolve the mechanism of storm-time relativistic electron precipitation, for which electromagnetic ion cyclotron (EMIC) waves are a prime candidate. From its ionospheric vantage point, ELFIN uses its unique pitch-angle-resolving capability to determine whether measured relativistic electron pitch-angle and energy spectra within the loss cone bear the characteristic signatures of scattering by EMIC waves or whether such scattering may be due to other processes. Pairing identical ELFIN satellites with slowly-variable along-track separation allows disambiguation of spatial and temporal evolution of the precipitation over minutes-to-tens-of-minutes timescales, faster than the orbit period of a single low-altitude satellite (~90min). Each satellite carries an energetic particle detector for electrons (EPDE) that measures 50keV to 5MeV electrons with deltaE/E, Submitted to Space Science Reviews April 2020. 51 pages, 7 tables, 21 figures
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- 2020
8. Physical Processes of Meso-Scale, Dynamic Auroral Forms
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Yukitoshi Nishimura, B. Gallardo-Lacourt, V. A. Sergeev, C. Forsyth, and Michael G. Henderson
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Meso scale ,Planetary science ,Field (physics) ,Space and Planetary Science ,Magnetosphere ,Astronomy and Astrophysics ,Geophysics ,Geology - Abstract
Meso-scale auroral forms, such as poleward boundary intensifications, streamers, omega bands, beads and giant undulations, are manifestations of dynamic processes in the magnetosphere driven, to a large part, by plasma instabilities in the magnetotail. New observations from ground- and space-based instrumentation and theoretical treatments are giving us a clearer view of some of the physical processes behind these auroral forms. However, questions remain as to how some of these observations should be interpreted, given uncertainties in mapping auroral features to locations in the magnetotatil and due to the significant overlap in the results from a variety of models of different plasma instabilities. We provide an overview of recent results in the field and seek to clarify some of the remaining questions with regards to what drives some of the largest and most dynamic auroral forms.
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- 2020
9. Solar wind dependence of electric conductances and currents in the auroral zone
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V. A. Sergeev, N. Stepanov, Kirsti Kauristie, Yasunobu Ogawa, and S. Käki
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Physics ,Atmospheric Science ,010504 meteorology & atmospheric sciences ,Magnetometer ,Incoherent scatter ,Conductance ,Sense (electronics) ,Conductivity ,010502 geochemistry & geophysics ,Atmospheric sciences ,01 natural sciences ,law.invention ,Solar wind ,Geophysics ,Space and Planetary Science ,law ,Electric field ,Ionosphere ,Atomic physics ,0105 earth and related environmental sciences - Abstract
Based on 20 years-long data base of EISCAT incoherent scatter radar and IMAGE magnetometer observations in Scandinavia, we investigate statistically the ionospheric conductance variations in the dark nightside auroral zone. We focus on the relationship of precipitation-caused conductances with the variations of local equivalent current and global AL index, as well as on their dependence on the solar wind (SW) parameters. In terms of paired correlation, the main SW drivers for AL index and for the Pedersen and Hall conductances ( Σ P and Σ H ) are the SW merging electric field (characterized, e.g., with the Kan-Lee function, E k l ) and the solar wind velocity V s w . The relative importance of these SW drivers varies. Whereas E k l is the main driver of AL index, the role of V s w increases for the conductances so that it outruns the E k l as the main driver for the Hall conductance. Quantitatively this dependence is represented as Σ H = ( 7.7 * V + 1.75 * V 2 ) + ( 5.7 * E − 0.86 * E 2 ) − 6.1 Siemens, where E and V are E k l and V s w normalized with E k l > = 0.79 mV/m and V s w > = 429 km/s. The strongest influence of V s w is, however, observed for the Hall-to-Pedersen conductance ratio R H P = Σ H / Σ P , indicating solar wind velocity control of the electron acceleration. Physically the energization is a major factor which contributes to the large conductance values. On the nightside, local equivalent currents are significantly controlled by the local Hall conductance (CC = 0.78) and most of the equivalent current increase during active periods is due to the conductivity change. In that sense the AL index variations during active times are controlled by the Hall conductance variations which, to a large extent, are controlled by the processes of magnetospheric electron acceleration.
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- 2018
10. Magnetotail Configuration During a Steady Convection Event as Observed by Low-Altitude and Magnetospheric Spacecraft
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Andrei Runov, Nikolai A. Tsyganenko, Howard J. Singer, Vassilis Angelopoulos, and V. A. Sergeev
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Low altitude ,Physics ,Convection ,010504 meteorology & atmospheric sciences ,Spacecraft ,business.industry ,Event (relativity) ,Geophysics ,01 natural sciences ,Current sheet ,Space and Planetary Science ,0103 physical sciences ,business ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences - Published
- 2018
11. First Measurement of the Hubble Constant from a Dark Standard Siren using the Dark Energy Survey Galaxies and the LIGO/Virgo Binary-Black-hole Merger GW170814
- Author
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Soares-Santos, M, Palmese, A, Hartley, W, Annis, J, Garcia-Bellido, J, Lahav, O, Doctor, Z, Fishbach, M, Holz, D. E, Lin, H, Pereira, M. E. S, Garcia, A, Herner, K, Kessler, R, Peiris, V, H, Sako, M, Allam, S, Brout, D, Carnero Rosell, A, Chen, H. Y, Conselice, C, Derose, J, Devicente, J, Diehl, H. T, Gill, M. S. S, Gschwend, J, Sevilla-Noarbe, I and Tucker, D. L., Wechsler, R, Berger, E, Cowperthwaite, P. S, Metzger, B. D, Williams, P. K. G, Abbott, T. M. C, Abdalla, F. B, Avila, S, Bechtol, K, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, D. L, Kind, Carrasco and Carretero, M., J, Castander, F. J, Crocce, M, Cunha, C. E, D'Andrea, C. B, da Costa, L. N, Davis, C, Desai, S, Doel, P, Drlica-Wagner, A, Eifler, T. F, Evrard, A. E, Flaugher, B, Fosalba, P, Frieman, J, Gaztanaga, E, Gerdes, D. W, Gruen, D, Gruendl, R. A, Gutierrez, G, Hollowood, D. L, Hoyle, B, James, D. J, Jeltema, T, Kuehn, K, Kuropatkin, N, T. S, Li, Lima, M, Maia, M. A. G, Marshall, J. L, Menanteau, F, Miquel, R, Neilsen, E, Ogando, R. L. C, Plazas, A. A, Romer, A. K, Roodman, A, Sanchez, E, Scarpine, V and Schindler, R, Schubnell, M, Serrano, S, Smith, M, Smith, R. C, Sobreira, F, Suchyta, E, Swanson, M. E. C, Tarle, G, Thomas, R. C, Walker, A. R, Wester, W, Zuntz, J, Abbott, B. P, Abbott, R, Abbott, T. D, Abraham, S, Acernese, F, Ackley, K, Adams, C, Adhikari, R. X, Adya, V. B, Affeldt, C, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O. D, Aiello, L, Ain, A, Ajith, P, Allen, G, Allocca, A, Aloy, M. A, Altin, P. A, Amato, A, Ananyeva, A, Anderson, S. B, Anderson, W. G, Angelova, S, Appert, S, Arai, K, Araya, M. C, Areeda, J. S, Arene, M, Ascenzi, S, Ashton, G, Aston, S. M, Astone, P, Aubin, F, Aufmuth, P, Aultoneal, K, Austin, C, Avendano, V and Avila-Alvarez, A, Babak, S, Bacon, P, Badaracco, F, Bader, M. K. M, Bae, S, Baker, P. T, Baldaccini, F, Ballardin, G, Ballmer, S. W, Banagiri, S, Barayoga, J. C, Barclay, S. E, Barish, B. C, Barker, D, Barkett, K, Barnum, S, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Bartos, I and Bassiri, Basti, A, Bawaj, M, Bayley, J. C, Bazzan, M, Becsy, B, Bejger, M, Bell, A. S, Beniwal, D, Bergmann, G, Bernuzzi, S, Bero, J. J, Berry, C. P. L, Bersanetti, D, Bertolini, A, Betzwieser, J, Bhandare, R, Bidler, J, Bilenko, I. A, Bilgili, S. A, Billingsley, G, Birch, J, Birney, R, Birnholtz, O, Biscans, S, Biscoveanu, S, Bisht, A, Bitossi, M, Blackburn, J. K, Blair, C. D, Blair, D. G, Blair, R. M, Bloemen, S, Bode, N, Boer, M, Boetzel, Y, Bogaert, G, Bondu, F, Bonilla, E, Bonnand, R, Booker, P, Boom, B. A, Booth, C. D, Bork, R, Boschi, V and Bose, Bossie, K, Bossilkov, V and Bosveld, Bouffanais, Y, Bozzi, A, Bradaschia, C, Brady, P. R, Bramley, A, Branchesi, M, Brau, J. E, Briant, T, Briggs, J. H, Brighenti, F, Brillet, A, Brinkmann, M, Brockill, P, Brooks, A. F, Brown, D. D, Brunett, S, Buikema, A, Bulik, T, Bulten, H. J, Buonanno, A, Buskulic, D, Buy, C, Byer, R. L, Cabero, M, Cadonati, L, Cagnoli, G, Cahillane, C, Bustillo, Calderon and Callister, J., T. A., Calloni, E, Camp, J. B, Campbell, W. A, Cannon, K. C, Cao, H, Cao, J, Capocasa, E, Carbognani, F, Caride, S, Carney, M. F, Carullo, G, Diaz, Casanueva and Casentini, J., C, Caudill, S, Cavaglia, M, Cavalieri, R, Cella, G, Cerda-Duran, P, Cerretani, G, Cesarini, E, Chaibi, O, Chakravarti, K, Chamberlin, S. J, Chan, M, Chao, S, Charlton, P, Chase, E. A, Chassande-Mottin, E, Chatterjee, D, Chaturvedi, M, Chatziioannou, K, Cheeseboro, B. D, Chen, X, Chen, Y, Cheng, H-P and Cheong, C. K., Chia, H. Y, Chincarini, A, Chiummo, A, Cho, G, Cho, H. S, Cho, M, Christensen, N, Chu, Q, Chua, S, Chung, K. W, Chung, S, Ciani, G, Ciobanu, A. A, Ciolfi, R, Cipriano, F, Cirone, A, Clara, F, Clark, J. A, Clearwater, P, Cleva, F, Cocchieri, C, Coccia, E, Colgan, R, Colleoni, M, Collette, C. G, Collins, C, Cominsky, L. R, Constancio Jr, M, Conti, L, Cooper, S. J, Corban, P, Corbitt, T. R, Cordero-Carrion, I and Corley, K. R., Cornish, N, Corsi, A, Cortese, S, Costa, C. A, Cotesta, R, Coughlin, M. W, Coughlin, S. B, Coulon, J-P and Countryman, S. T., Couvares, P, Covas, P. B, Cowan, E. E, Coward, D. M, Cowart, M. J, Coyne, D. C, Coyne, R, Creighton, J. D. E, Creighton, T. D, Cripe, J, Croquette, M, Crowder, S. G, Cullen, T. J, Cumming, A, Cunningham, L, Cuoco, E, Dal Canton, T, Dalya, G, D'Antonio, S, Danilishin, S. L, Danzmann, K, Dasgupta, A, Costa, Da Silva and Datrier, C. F., L. E. H., Dattilo, V and Dave, I and Davis, D, Daw, E. J, Debra, D, Deenadayalan, M, Degallaix, J, De Laurentis, M, Deleglise, S, Del Pozzo, W, Demarchi, L. M, Demos, N, Dent, T, De Pietri, R, Derby, J, De Rosa, R, De Rossi, C, Desalvo, R, de Varona, O, Dhurandhar, S, Diaz, M. C, Dietrich, T, Di Fiore, L, Di Giovanni, M, Di Girolamo, T, Di Lieto, A, Ding, B, Di Pace, S, Palma, Di, I and Di Renzo, F, Dmitriev, A, Donovan, F, Dooley, K. L, Doravari, S, Dorrington, I and Downes, T. P., Drago, M, Driggers, J. C, Du, Z, Dupej, P, Dwyer, S. E, Easter, P. J, Edo, T. B, Edwards, M. C, Effler, A, Ehrens, P, Eichholz, J, Eikenberry, S. S, Eisenmann, M, Eisenstein, R. A, Estelles, H, Estevez, D, Etienne, Z. B, Etzel, T, Evans, M, Evans, T. M, Fafone, V and Fair, Fairhurst, S, Fan, X, Farinon, S, Farr, B, Farr, W. M, Fauchon-Jones, E. J, Favata, M, Fays, M, Fazio, M, Fee, C, Feicht, J, Fejer, M. M, Feng, F, Fernandez-Galiana, A, Ferrante, I and Ferreira, E. C., Ferreira, T. A, Ferrini, F, Fidecaro, F, Fiori, I and Fiorucci, Fisher, R. P, Fishner, J. M, Fitz-Axen, M, Flaminio, R, Fletcher, M, Flynn, E, Fong, H, Fournier, J-D and Font, J. A., Forsyth, P. W. F, Frasca, S, Frasconi, F, Frei, Z, Freise, A, Frey, R, Fritschel, P, Frolov, V. V, Fulda, P, Fyffe, M, Gabbard, H. A, Gadre, B. U, Gaebel, S. M, Gair, J. R, Gammaitoni, L, Ganija, M. R, Gaonkar, S. 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A, Khursheed, M, Kijbunchoo, N, Kim, Chunglee and Kim, J. C., Kim, K, Y-M and Kim, W, Kim, W. S, Kimball, C, King, E. J, King, P. J, Kinley-Hanlon, M, Kirchhoff, R, Kissel, J. S, Kleybolte, L, Klika, J. H, Klimenko, S, Knowles, T. D, Koch, P, Koehlenbeck, S. M, Koekoek, G, Koley, S, Kondrashov, V and Kontos, Koper, N, Korobko, M, Korth, W. Z, Kowalska, I and Kozak, D. B., Kringel, V and Krishnendu, Krolak, A, Kuehn, G, Kumar, A, Kumar, P, Kumar, R, Kumar, S, Kuo, L, Kutynia, A, Kwang, S, Lackey, B. D, Lai, K. H, Lam, T. L, Landry, M, Lane, B. B, Lang, R. N, Lange, J, Lantz, B, Lanza, R. K, Lasky, P. D, Laxen, M, Lazzarini, A, Lazzaro, C, Leaci, P, Leavey, S, Lecoeuche, Y. K, Lee, C. H, Lee, H. K, Lee, H. M, Lee, H. W, Lee, J, Lee, K, Lehmann, J, Lenon, A, Letendre, N, Levin, Y, Li, J, K. J. L, Li, T. G. F, Li, Li, X, Lin, F, Linde, F, Linker, S. D, Littenberg, T. B, Liu, J, Liu, X, R. K. L, Lo, Lockerbie, N. A, London, L. 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Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), ITA, USA, GBR, FRA, DEU, ESP, RS: FSE Grav. waves and fundamental physics, Grav. waves and fundamental physics, RS: FSE MSP, Soares-Santos, M., Palmese, A., Hartley, W., Annis, J., Garcia-Bellido, J., Lahav, O., Doctor, Z., Fishbach, M., Holz, D. 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J., Moraru, D., Moreno, G., Morisaki, S., Mours, B., Mow-Lowry, C. M., Mukherjee, Arunava, Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Muñiz, E. A., Muratore, M., Murray, P. G., Nardecchia, I., Naticchioni, L., Nayak, R. K., Neilson, J., Nelemans, G., Nelson, T. J. N., Nery, M., Neunzert, A., Ng, K. Y., Ng, S., Nguyen, P., Nichols, D., Nissanke, S., Nocera, F., North, C., Nuttall, L. K., Obergaulinger, M., Oberling, J., O’Brien, B. D., O’Dea, G. D., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Ohta, H., Okada, M. A., Oliver, M., Oppermann, P., Oram, Richard J., O’Reilly, B., Ormiston, R. G., Ortega, L. F., O’Shaughnessy, R., Ossokine, S., Ottaway, D. J., Overmier, H., Owen, B. J., Pace, A. E., Pagano, G., Page, M. A., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pal-Singh, A., Pan, Huang-Wei, Pang, B., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Parida, A., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patil, M., Patricelli, B., Pearlstone, B. L., Pedersen, C., Pedraza, M., Pedurand, R., Pele, A., Penn, S., Perez, C. J., Perreca, A., Pfeiffer, H. P., Phelps, M., Phukon, K. S., Piccinni, O. J., Pichot, M., Piergiovanni, F., Pillant, G., Pinard, L., Pirello, M., Pitkin, M., Poggiani, R., Pong, D. Y. T., Ponrathnam, S., Popolizio, P., Porter, E. K., Powell, J., Prajapati, A. K., Prasad, J., Prasai, K., Prasanna, R., Pratten, G., Prestegard, T., Privitera, S., Prodi, G. A., Prokhorov, L. G., Puncken, O., Punturo, M., Puppo, P., Pürrer, M., Qi, H., Quetschke, V., Quinonez, P. J., Quintero, E. A., Quitzow-James, R., Radkins, H., Radulescu, N., Raffai, P., Raja, S., Rajan, C., Rajbhandari, B., Rakhmanov, M., Ramirez, K. E., Ramos-Buades, A., Rana, Javed, Rao, K., Rapagnani, P., Raymond, V., Razzano, M., Read, J., Regimbau, T., Rei, L., Reid, S., Reitze, D. 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E., Zweizig, J., Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-École Nationale Supérieure des Sciences Appliquées et de Technologie (ENSSAT)-Centre National de la Recherche Scientifique (CNRS)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Collège de France (CdF (institution))
- Subjects
010504 meteorology & atmospheric sciences ,Astronomy ,Astrophysics ,cosmic background radiation ,01 natural sciences ,black hole ,LIGO ,dark energy ,010303 astronomy & astrophysics ,gravitational wave ,QC ,Photometric redshift ,QB ,Physics ,Settore FIS/01 ,Hubble constant ,CATALOG ,observations [cosmology] ,gravitational waves ,Physical Sciences ,symbols ,astro-ph.CO ,STELLAR MASS ,Astrophysics - Cosmology and Nongalactic Astrophysics ,observation [cosmology] ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Astrophysics::High Energy Astrophysical Phenomena ,AST-1138766 ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astronomy & Astrophysics ,gravitational radiation: direct detection ,electromagnetic field: production ,symbols.namesake ,SDG 17 - Partnerships for the Goals ,Binary black hole ,statistical analysis ,surveys ,0103 physical sciences ,supernova ,AST-1536171 ,Luminosity distance ,STFC ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences ,ONDAS GRAVITACIONAIS ,Science & Technology ,catalogs ,cosmology: observations ,gravitational radiation ,RCUK ,Astronomy and Astrophysics ,redshift ,Galaxy ,Redshift ,gravitational radiation detector ,VIRGO ,Physics and Astronomy ,black hole: binary ,RESOLUTION ,Space and Planetary Science ,gravitational radiation: emission ,Dark energy ,galaxy ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Hubble's law - Abstract
We present a multi-messenger measurement of the Hubble constant H_0 using the binary-black-hole merger GW170814 as a standard siren, combined with a photometric redshift catalog from the Dark Energy Survey (DES). The luminosity distance is obtained from the gravitational wave signal detected by the LIGO/Virgo Collaboration (LVC) on 2017 August 14, and the redshift information is provided by the DES Year 3 data. Black-hole mergers such as GW170814 are expected to lack bright electromagnetic emission to uniquely identify their host galaxies and build an object-by-object Hubble diagram. However, they are suitable for a statistical measurement, provided that a galaxy catalog of adequate depth and redshift completion is available. Here we present the first Hubble parameter measurement using a black-hole merger. Our analysis results in $H_0 = 75.2^{+39.5}_{-32.4}~{\rm km~s^{-1}~Mpc^{-1}}$, which is consistent with both SN Ia and CMB measurements of the Hubble constant. The quoted 68% credible region comprises 60% of the uniform prior range [20,140] ${\rm km~s^{-1}~Mpc^{-1}}$, and it depends on the assumed prior range. If we take a broader prior of [10,220] ${\rm km~s^{-1}~Mpc^{-1}}$, we find $H_0 = 78^{+ 96}_{-24}~{\rm km~s^{-1}~Mpc^{-1}}$ ($57\%$ of the prior range). Although a weak constraint on the Hubble constant from a single event is expected using the dark siren method, a multifold increase in the LVC event rate is anticipated in the coming years and combinations of many sirens will lead to improved constraints on $H_0$., Comment: 18 pages, 2 Figures, submitted to ApJL
- Published
- 2019
12. Search for Multimessenger Sources of Gravitational Waves and High-energy Neutrinos with Advanced LIGO during Its First Observing Run, ANTARES, and IceCube
- Author
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A, Clearwater, P, Cleva, F, Cocchieri, C, Coccia, E, Cohadon, P-F and Cohen, Colgan, R, Colleoni, M, Collette, C. G, Collins, C, Cominsky, L. R, Constancio Jr, M, Conti, L, Cooper, S. J, Corban, P, Corbitt, T. R, Cordero-Carrion, I and Corley, K. R., Cornish, N, Corsi, A, Cortese, S, Costa, C. A, Cotesta, R, Coughlin, M. W, Coughlin, S. B, Coulon, J-P and Countryman, S. T., Couvares, P, Covas, P. B, Cowan, E. E, Coward, D. M, Cowart, M. J, Coyne, D. C, Coyne, R, Creighton, J. D. E, Creighton, T. D, Cripe, J, Croquette, M, Crowder, S. G, Cullen, T. J, Cumming, A, Cunningham, L, Cuoco, E, Dal Canton, T, Dalya, G, Danilishin, S. L, D'Antonio, S, Danzmann, K, Dasgupta, A, Costa, Da Silva and Datrier, C. F., L. E. H., Dattilo, V and Dave, I and Davier, Davis, D, Daw, E. J, Debra, D, Deenadayalan, M, Degallaix, J, De Laurentis, M, Deleglise, S, Del Pozzo, W, Demarchi, L. M, Demos, N, Dent, T, Denys, M, De Pietri, R, Derby, J, De Rosa, R, De Rossi, C, Desalvo, R, de Varona, O, Dhurandhar, S, Diaz, M. C, Dietrich, T, Di Fiore, L, Di Giovanni, M, Di Girolamo, T, Di Lieto, A, Ding, B, Di Pace, S, Di Renzo, F, Dmitriev, A, Doctor, Z, Donovan, F, Dooley, K. L, Doravari, S, Dorrington, I and Downes, T. P., Drago, M, Driggers, J. C, Du, Z, Ducoin, J-G and Dupej, Dwyer, S. E, Easter, P. J, Edo, T. B, Edwards, M. C, Effler, A, Ehrens, P, Eichholz, J, Eikenberry, S. S, Eisenmann, M, Eisenstein, R. A, Essick, R. C, Estelles, H, Estevez, D, Etienne, Z. B, Etzel, T, Evans, M, Evans, T. M, Fafone, V and Fair, Fairhurst, S, Fan, X, Farinon, S, Farr, B, Farr, W. M, Fauchon-Jones, E. J, Favata, M, Fays, M, Fazio, M, Fee, C, Feicht, J, Fejer, M. M, Feng, F, Fernandez-Galiana, A, Ferrante, I and Ferreira, E. C., Ferreira, T. A, Ferrini, F, Fidecaro, F, Fiori, I and Fiorucci, Fishbach, M, Fisher, R. P, Fishner, J. M, Fitz-Axen, M, Flaminio, R, Fletcher, M, Flynn, E, Fong, H, Font, J. A, Forsyth, P. W. F, Fournier, J-D and Frasca, Frasconi, F, Frei, Z, Freise, A, Frey, R, Frey, V and Fritschel, Frolov, V. V, Fulda, P, Fyffe, M, Gabbard, H. A, Gadre, B. U, Gaebel, S. M, Gair, J. R, Gammaitoni, L, Ganija, M. R, Gaonkar, S. G, Garcia, A, Garcia-Quiros, C, Garufi, F, Gateley, B, Gaudio, S, Gaur, G, Gayathri, V and Gemme, Genin, E, Gennai, A, George, D, George, J, Gergely, L, Germain, V and Ghonge, Ghosh, Abhirup and Ghosh, Archisman and Ghosh, Giacomazzo, B, Giaime, J. A, Giardina, K. D, Giazotto, A, Gill, K, Giordano, G, Glover, L, Godwin, P, Goetz, E, Goetz, R, Goncharov, B, Gonzalez, G, Castro, Gonzalez and Gopakumar, J. M., Gorodetsky, M. L, Gossan, S. E, Gosselin, M, Gouaty, R, Grado, A, Graef, C, Granata, M, Grant, A, Gras, S, Grassia, P, Gray, C, Gray, R, Greco, G, Green, A. C, Green, R, Gretarsson, E. M, Groot, P, Grote, H, Grunewald, S, Gruning, P, Guidi, G. M, Gulati, H. K, Guo, Y, Gupta, A, Gupta, M. K, Gustafson, E. K, Gustafson, R, Haegel, L, Halim, O, Hall, B. R, Hall, E. D, Hamilton, E. Z, Hammond, G, Haney, M, Hanke, M. M, Hanks, J, Hanna, C, Hannuksela, O. A, Hanson, J, Hardwick, T, Haris, K, Harms, J, Harry, G. M, Harry, I. W, Haster, C-J and Haughian, Hayes, F. J, Healy, J, Heidmann, A, Heintze, M. C, Heitmann, H, Hello, P, Hemming, G, Hendry, M, Heng, I. S, Hennig, J, Heptonstall, A. W, Hernandez, F. J, Heurs, M, Hild, S, Hinderer, T, Hoak, D, Hochheim, S, Hofman, D, Holgado, A. M, Holland, N. A, Holt, K, Holz, D. E, Hopkins, P, Horst, C, Hough, J, Howell, E. J, Hoy, C. G, Hreibi, A, Huerta, E. A, Huet, D, Hughey, B, Hulko, M, Husa, S, Huttner, S. H, Huynh-Dinh, T, Idzkowski, B, Iess, A, Ingram, C, Inta, R, Intini, G, Irwin, B, Isa, H. N, Isac, J-M and Isi, Iyer, B. R, Izumi, K, Jacqmin, T, Jadhav, S. J, Jani, K, Janthalur, N. N, Jaranowski, P, Jenkins, A. C, Jiang, J, Johnson, D. S, Jones, A. W, Jones, I, Jones, R, Jonker, R. J. G, Ju, L, Junker, J, Kalaghatgi, Kalogera, V and Kamai, B, Kandhasamy, S, Kang, G, Kanner, J. B, Kapadia, S. J, Karki, S, Karvinen, K. S, Kashyap, R, Kasprzack, M, Katsanevas, S, Katsavounidis, E, Katzman, W, Kaufer, S, Kawabe, K, Keerthana, Kefelian, F, Keitel, D, Kennedy, R, Key, J. S, Khalili, F. Y, Khan, H, Khan, I and Khan, Khan, Z, Khazanov, E. A, Khursheed, M, Kijbunchoo, N, Kim, Chunglee and Kim, J. C., Kim, K, Kim, W, Kim, W. S, Y-M and Kimball, King, E. J, King, P. J, Kinley-Hanlon, M, Kirchhoff, R, Kissel, J. S, Kleybolte, L, Klika, J. H, Klimenko, S, Knowles, T. D, Koch, P, Koehlenbeck, S. M, Koekoek, G, Koley, S, Kondrashov, V and Kontos, Koper, N, Korobko, M, Korth, W. Z, Kowalska, I and Kozak, D. B., Kringel, V and Krishnendu, Krolak, A, Kuehn, G, Kumar, A, Kumar, P, Kumar, R, Kumar, S, Kuo, L, Kutynia, A, Kwang, S, Lackey, B. D, Lai, K. H, Lam, T. L, Landry, M, Lane, B. B, Lang, R. N, Lange, J, Lantz, B, Lanza, R. K, Lartaux-Vollard, A, Lasky, P. D, Laxen, M, Lazzarini, A, Lazzaro, C, Leaci, P, Leavey, S, Lecoeuche, Y. K, Lee, C. H, Lee, H. K, Lee, H. M, Lee, H. W, Lee, J, Lee, K, Lehmann, J, Lenon, A, Leroy, N, Letendre, N, Levin, Y, Li, J, K. J. L, Li, T. G. F, Li, Li, X, Lin, F, Linde, F, Linker, S. D, Littenberg, T. B, Liu, J, Liu, X, R. K. L, Lo, Lockerbie, N. A, London, L. T, Longo, A, Lorenzini, M, Loriette, V and Lormand, Losurdo, G, Lough, J. D, Lousto, C. O, Lovelace, G, Lower, M. E, Lueck, H, Lumaca, D, Lundgren, A. P, Lynch, R, Ma, Y, Macas, R, Macfoy, S, Macinnis, M, Macleod, D. M, Macquet, A, Magana-Sandoval, F, Zertuche, Magana and Magee, L., R. M., Majorana, E, Maksimovic, I and Malik, Man, N, Mandic, V and Mangano, V and Mansell, G. L., Manske, M, Mantovani, M, Marchesoni, F, Marion, F, Marka, S, Marka, Z, Markakis, C, Markosyan, A. S, Markowitz, A, Maros, E, Marquina, A, Marsat, S, Martelli, F, Martin, I. W, Martin, R. M, Martynov, Mason, K, Massera, E, Masserot, A, Massinger, T. 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ENS Paris (FRDPENS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Albert, A., André, M., Anghinolfi, M., Ardid, M., Aubert, J. -J., Aublin, J., Avgitas, T., Baret, B., Barrios-Martí, J., Basa, S., Belhorma, B., Bertin, V., Biagi, S., Bormuth, R., Boumaaza, J., Bourret, S., Bouwhuis, M. C., Brânzaş, H., Bruijn, R., Brunner, J., Busto, J., Capone, A., Caramete, L., Carr, J., Celli, S., Chabab, M., El Moursli, R. Cherkaoui, Chiarusi, T., Circella, M., Coelho, J. A. B., Coleiro, A., Colomer, M., Coniglione, R., Costantini, H., Coyle, P., Creusot, A., Díaz, A. F., Deschamps, A., Distefano, C., Di Palma, I., Domi, A., Donà, R., Donzaud, C., Dornic, D., Drouhin, D., Eberl, T., El Bojaddaini, I., El Khayati, N., Elsässer, D., Enzenhöfer, A., Ettahiri, A., Fassi, F., Felis, I., Fermani, P., Ferrara, G., Fusco, L., Gay, P., Glotin, H., Grégoire, T., Ruiz, R. Gracia, Graf, K., Hallmann, S., Van Haren, H., Heijboer, A. J., Hello, Y., Hernández-Rey, J. J., Hößl, J., Hofestädt, J., Illuminati, G., De Jong, M., Jongen, M., Kadler, M., Kalekin, O., Katz, U., Khan-Chowdhury, N. R., Kouchner, A., Kreter, M., Kreykenbohm, I., Kulikovskiy, V., Lachaud, C., Lahmann, R., Lefèvre, D., Leonora, E., Levi, G., Lotze, M., Loucatos, S., Maggi, G., Marcelin, M., Margiotta, A., Marinelli, A., Martínez-Mora, J. A., Mele, R., Melis, K., Migliozzi, P., Moussa, A., Navas, S., Nezri, E., Nuñez, A., Organokov, M., Pǎvǎlaş, G. E., Pellegrino, C., Piattelli, P., Popa, V., Pradier, T., Quinn, L., Racca, C., Randazzo, N., Riccobene, G., Sánchez-Losa, A., Saldaña, M., Salvadori, I., Samtleben, D. F. E., Sanguineti, M., Sapienza, P., Schüssler, F., Spurio, M., Stolarczyk, Th., Taiuti, M., Tayalati, Y., Trovato, A., Vallage, B., Van Elewyck, V., Versari, F., Vivolo, D., Wilms, J., Zaborov, D., Zornoza, J. D., Zñiga, J., Aartsen, M. G., Ackermann, M., Adams, J., Aguilar, J. A., Ahlers, M., Ahrens, M., Altmann, D., Andeen, K., Anderson, T., Ansseau, I., Anton, G., Argüelles, C., Auffenberg, J., Axani, S., Backes, P., Bagherpour, H., Bai, X., Barbano, A., Barron, J. P., Barwick, S. W., Baum, V., Bay, R., Beatty, J. J., Tjus, J. Becker, Becker, K. -H., Benzvi, S., Berley, D., Bernardini, E., Besson, D. Z., Binder, G., Bindig, D., Blaufuss, E., Blot, S., Bohm, C., Börner, M., Bos, F., Böser, S., Botner, O., Bourbeau, E., Bourbeau, J., Bradascio, F., Braun, J., Brenzke, M., Bretz, H. -P., Bron, S., Brostean-Kaiser, J., Burgman, A., Busse, R. S., Carver, T., Cheung, E., Chirkin, D., Clark, K., Classen, L., Collin, G. H., Conrad, J. M., Coppin, P., Correa, P., Cowen, D. F., Cross, R., Dave, P., Day, M., De André, J. P. A. M., De Clercq, C., Delaunay, J. J., Dembinski, H., Deoskar, K., De Ridder, S., Desiati, P., De Vries, K. D., De Wasseige, G., De With, M., Deyoung, T., Díaz-Vélez, J. C., Lorenzo, V. Di, Dujmovic, H., Dumm, J. P., Dunkman, M., Dvorak, E., Eberhardt, B., Ehrhardt, T., Eichmann, B., Eller, P., Evenson, P. A., Fahey, S., Fazely, A. R., Felde, J., Filimonov, K., Finley, C., Franckowiak, A., Friedman, E., Fritz, A., Gaisser, T. K., Gallagher, J., Ganster, E., Garrappa, S., Gerhardt, L., Ghorbani, K., Giang, W., Glauch, T., Glüsenkamp, T., Goldschmidt, A., Gonzalez, J. G., Grant, D., Griffith, Z., Haack, C., Hallgren, A., Halve, L., Halzen, F., Hanson, K., Hebecker, D., Heereman, D., Helbing, K., Hellauer, R., Hickford, S., Hignight, J., Hill, G. C., Hoffman, K. D., Hoffmann, R., Hoinka, T., Hokanson-Fasig, B., Hoshina, K., Huang, F., Huber, M., Hultqvist, K., Hünnefeld, M., Hussain, R., In, S., Iovine, N., Ishihara, A., Jacobi, E., Japaridze, G. S., Jeong, M., Jero, K., Jones, B. J. P., Kalaczynski, P., Kang, W., Kappes, A., Kappesser, D., Karg, T., Karle, A., Kauer, M., Keivani, A., Kelley, J. L., Kheirandish, A., Kim, J., Kintscher, T., Kiryluk, J., Kittler, T., Klein, S. R., Koirala, R., Kolanoski, H., Köpke, L., Kopper, C., Kopper, S., Koschinsky, J. P., Koskinen, D. J., Kowalski, M., Krings, K., Kroll, M., Krückl, G., Kunwar, S., Kurahashi, N., Kyriacou, A., Labare, M., Lanfranchi, J. L., Larson, M. J., Lauber, F., Leonard, K., Leuermann, M., Liu, Q. R., Lohfink, E., Mariscal, C. J. Lozano, Lu, L., Lünemann, J., Luszczak, W., Madsen, J., Mahn, K. B. M., Makino, Y., Mancina, S., Mariş, I. C., Maruyama, R., Mase, K., Maunu, R., Meagher, K., Medici, M., Meier, M., Menne, T., Merino, G., Meures, T., Miarecki, S., Micallef, J., Momenté, G., Montaruli, T., Moore, R. W., Moulai, M., Nagai, R., Nahnhauer, R., Nakarmi, P., Naumann, U., Neer, G., Niederhausen, H., Nowicki, S. C., Nygren, D. R., Pollmann, A. Obertacke, Olivas, A., O'Murchadha, A., O'Sullivan, E., Palczewski, T., Pandya, H., Pankova, D. V., Peiffer, P., Pepper, J. A., De Los Heros, C. Pérez, Pieloth, D., Pinat, E., Pizzuto, A., Plum, M., Price, P. B., Przybylski, G. T., Raab, C., Rameez, M., Rauch, L., Rawlins, K., Rea, I. C., Reimann, R., Relethford, B., Renzi, G., Resconi, E., Rhode, W., Richman, M., Robertson, S., Rongen, M., Rott, C., Ruhe, T., Ryckbosch, D., Rysewyk, D., Safa, I., Herrera, S. E. Sanchez, Sandrock, A., Sandroos, J., Santander, M., Sarkar, S., Satalecka, K., Schaufel, M., Schlunder, P., Schmidt, T., Schneider, A., Schneider, J., Schöneberg, S., Schumacher, L., Sclafani, S., Seckel, D., Seunarine, S., Soedingrekso, J., Soldin, D., Song, M., Spiczak, G. M., Spiering, C., Stachurska, J., Stamatikos, M., Stanev, T., Stasik, A., Stein, R., Stettner, J., Steuer, A., Stezelberger, T., Stokstad, R. G., Stößl, A., Strotjohann, N. L., Stuttard, T., Sullivan, G. W., Sutherland, M., Taboada, I., Tenholt, F., Ter-Antonyan, S., Terliuk, A., Tilav, S., Toale, P. A., Tobin, M. N., Tönnis, C., Toscano, S., Tosi, D., Tselengidou, M., Tung, C. F., Turcati, A., Turcotte, R., Turley, C. F., Ty, B., Unger, E., Elorrieta, M. A. Unland, Usner, M., Vandenbroucke, J., Van Driessche, W., Van Eijk, D., Van Eijndhoven, N., Vanheule, S., Van Santen, J., Vraeghe, M., Walck, C., Wallace, A., Wallraff, M., Wandler, F. D., Wandkowsky, N., Watson, T. B., Waza, A., Weaver, C., Weiss, M. 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W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Bejger, M., Belahcene, I., Bell, A. S., Beniwal, D., Berger, B. K., Bergmann, G., Bernuzzi, S., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bidler, J., Bilenko, I. A., Bilgili, S. A., Billingsley, G., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Booth, C. D., Bork, R., Boschi, V., Bose, S., Bossie, K., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branchesi, M., Brau, J. E., Briant, T., Briggs, J. H., Brighenti, F., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. D., Brunett, S., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. Calderón, Callister, T. A., Calloni, E., Camp, J. B., Campbell, W. A., Cannon, K. C., Cao, H., Cao, J., Capocasa, E., Carbognani, F., Caride, S., Carney, M. F., Carullo, G., Diaz, J. Casanueva, Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cerdá-Durán, P., Cerretani, G., Cesarini, E., Chaibi, O., Chakravarti, K., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chase, E. A., Chassande-Mottin, E., Chatterjee, D., Chaturvedi, M., Cheeseboro, B. D., Chen, H. Y., Chen, X., Chen, Y., Cheng, H. -P., Cheong, C. K., Chia, H. Y., Chincarini, A., Chiummo, A., Cho, G., Cho, H. S., Cho, M., Christensen, N., Chu, Q., Chua, S., Chung, K. W., Chung, S., Ciani, G., Ciobanu, A. A., Ciolfi, R., Cipriano, F., Cirone, A., Clara, F., Clark, J. A., Clearwater, P., Cleva, F., Cocchieri, C., Coccia, E., Cohadon, P. -F., Cohen, D., Colgan, R., Colleoni, M., Collette, C. G., Collins, C., Cominsky, L. R., Constancio, M., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrión, I., Corley, K. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Cotesta, R., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Covas, P. B., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Cripe, J., Croquette, M., Crowder, S. G., Cullen, T. J., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Dálya, G., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dasgupta, A., Costa, C. F. Da Silva, Datrier, L. E. H., Dattilo, V., Dave, I., Davier, M., Davis, D., Daw, E. J., Debra, D., Deenadayalan, M., Degallaix, J., De Laurentis, M., Deléglise, S., Pozzo, W. Del, Demarchi, L. M., Demos, N., Dent, T., Denys, M., De Pietri, R., Derby, J., De Rosa, Rosario., De Rossi, C., Desalvo, R., De Varona, O., Dhurandhar, S., Díaz, M. C., Dietrich, T., Fiore, L. Di., Giovanni, M. Di., Di Girolamo, T., Lieto, A. Di., Ding, B., Pace, S. Di., Renzo, F. Di., Dmitriev, A., Doctor, Z., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Downes, T. P., Drago, M., Driggers, J. C., Du, Z., Ducoin, J. -G., Dupej, P., Dwyer, S. E., Easter, P. J., Edo, T. B., Edwards, M. C., Effler, A., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenmann, M., Eisenstein, R. A., Essick, R. C., Estelles, H., Estevez, D., Etienne, Z. B., Etzel, T., Evans, M., Evans, T. M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fazio, M., Fee, C., Feicht, J., Fejer, M. M., Feng, F., Fernandez-Galiana, A., Ferrante, I., Ferreira, E. C., Ferreira, T. A., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fishbach, M., Fisher, R. P., Fishner, J. M., Fitz-Axen, M., Flaminio, R., Fletcher, M., Flynn, E., Fong, H., Font, J. A., Forsyth, P. W. F., Fournier, J. -D., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H. A., Gadre, B. U., Gaebel, S. M., Gair, J. R., Gammaitoni, L., Ganija, M. R., Gaonkar, S. G., Garcia, A., García-Quirós, C., Garufi, F., Gateley, B., Gaudio, S., Gaur, G., Gayathri, V., Gemme, G., Genin, E., Gennai, A., George, D., George, J., Gergely, L., Germain, V., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, S., Giacomazzo, B., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Giordano, G., Glover, L., Godwin, P., Goetz, E., Goetz, R., Goncharov, B., González, G., Castro, J. M. Gonzalez, Gopakumar, A., Gorodetsky, M. L., Gossan, S. 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Perreca, A, Pfeiffer, H, Phelps, M, Phukon, K, Piccinni, O, Pichot, M, Piergiovanni, F, Pillant, G, Pinard, L, Pirello, M, Pitkin, M, Poggiani, R, Pong, D, Ponrathnam, S, Popolizio, P, Porter, E, Powell, J, Prajapati, A, Prasad, J, Prasai, K, Prasanna, R, Pratten, G, Prestegard, T, Privitera, S, Prodi, G, Prokhorov, L, Puncken, O, Punturo, M, Puppo, P, Pürrer, M, Qi, H, Quetschke, V, Quinonez, P, Quintero, E, Quitzow-James, R, Raab, F, Radkins, H, Radulescu, N, Raffai, P, Raja, S, Rajan, C, Rajbhandari, B, Rakhmanov, M, Ramirez, K, Ramos-Buades, A, Rana, J, Rao, K, Rapagnani, P, Raymond, V, Razzano, M, Read, J, Regimbau, T, Rei, L, Reid, S, Reitze, D, Ren, W, Ricci, F, Richardson, C, Richardson, J, Ricker, P, Riles, K, Rizzo, M, Robertson, N, Robie, R, Robinet, F, Rocchi, A, Rolland, L, Rollins, J, Roma, V, Romanelli, M, Romano, R, Romel, C, Romie, J, Rose, K, Rosińska, D, Rosofsky, S, Ross, M, Rowan, S, Rüdiger, A, Ruggi, P, Rutins, G, Ryan, K, Sachdev, S, Sadecki, T, Sakellariadou, M, Salconi, L, Saleem, M, Samajdar, A, Sammut, L, Sanchez, E, Sanchez, L, Sanchis-Gual, N, Sandberg, V, Sanders, J, Santiago, K, Sarin, N, Sassolas, B, Saulson, P, Sauter, O, Savage, R, Schale, P, Scheel, M, Scheuer, J, Schiettekatte, F, Schmidt, P, Schnabel, R, Schofield, R, Schönbeck, A, Schreiber, E, Schulte, B, Schutz, B, Schwalbe, S, Scott, J, Scott, S, Seidel, E, Sellers, D, Sengupta, A, Sennett, N, Sentenac, D, Sequino, V, Sergeev, A, Setyawati, Y, Shaddock, D, Shaffer, T, Shahriar, M, Shaner, M, Shao, L, Sharma, P, Shawhan, P, Shen, H, Shink, R, Shoemaker, D, Shyamsundar, S, Siellez, K, Sieniawska, M, Sigg, D, Silva, A, Singer, L, Singh, N, Singhal, A, Sintes, A, Sitmukhambetov, S, Skliris, V, Slagmolen, B, Slaven-Blair, T, Smith, J, Smith, R, Somala, S, Son, E, Sorazu, B, Sorrentino, F, Souradeep, T, Sowell, E, Spencer, A, Srivastava, A, Srivastava, V, Staats, K, Stachie, C, Standke, M, Steer, D, Steinke, M, Steinlechner, J, Steinlechner, S, Steinmeyer, D, Stevenson, S, Stocks, D, Stone, R, Stops, D, Strain, K, Stratta, G, Strigin, S, Strunk, A, Sturani, R, Stuver, A, Sudhir, V, Summerscales, T, Sun, L, Sunil, S, Suresh, J, Sutton, P, Swinkels, B, Szczepańczyk, M, Tacca, M, Tait, S, Talbot, C, Talukder, D, Tanner, D, Tápai, M, Taracchini, A, Tasson, J, Taylor, R, Thies, F, Thomas, M, Thomas, P, Thondapu, S, Thorne, K, Thrane, E, Tiwari, S, Tiwari, V, Toland, K, Tonelli, M, Tornasi, Z, Torres-Forné, A, Torrie, C, Töyrä, D, Travasso, F, Traylor, G, Tringali, M, Trozzo, L, Trudeau, R, Tsang, K, Tse, M, Tso, R, Tsukada, L, Tsuna, D, Tuyenbayev, D, Ueno, K, Ugolini, D, Unnikrishnan, C, Urban, A, Usman, S, Vahlbruch, H, Vajente, G, Valdes, G, Van Bakel, N, Van Beuzekom, M, Van Den Brand, J, Broeck, C, Vander-Hyde, D, Schaaf, L, Van Heijningen, J, Van Veggel, A, Vardaro, M, Varma, V, Vass, S, Vasúth, M, Vecchio, A, Vedovato, G, Veitch, J, Veitch, P, Venkateswara, K, Venugopalan, G, Verkindt, D, Vetrano, F, Viceré, A, Viets, A, Vine, D, Vinet, J, Vitale, S, Vo, T, Vocca, H, Vorvick, C, Vyatchanin, S, Wade, A, Wade, L, Wade, M, Walet, R, Walker, M, Wallace, L, Walsh, S, Wang, G, Wang, H, Wang, J, Wang, W, Wang, Y, Ward, R, Warden, Z, Warner, J, Was, M, Watchi, J, Weaver, B, Wei, L, Weinert, M, Weinstein, A, Weiss, R, Wellmann, F, Wen, L, Wessel, E, Weßels, P, Westhouse, J, Wette, K, Whelan, J, Whiting, B, Whittle, C, Wilken, D, Williamson, A, Willis, J, Willke, B, Wimmer, M, Winkler, W, Wipf, C, Wittel, H, Woan, G, Woehler, J, Wofford, J, Worden, J, Wright, J, Wu, D, Wysocki, D, Xiao, L, Yamamoto, H, Yancey, C, Yang, L, Yap, M, Yazback, M, Yeeles, D, Yu, H, Yuen, S, Yvert, M, Zadrozny, A, Zadrożny, A, Zanolin, M, Zelenova, T, Zendri, J, Zevin, M, Zhang, J, Zhang, L, Zhang, T, Zhao, C, Zhou, M, Zhou, Z, Zhu, X, Zucker, M, Zweizig, J, Andre, M., Barrios-Marti, J., Branzas, H., El Moursli, R. C., Diaz, A. F., Dona, R., Elsasser, D., Enzenhofer, A., Gregoire, T., Ruiz, R. G., Hernandez-Rey, J. J., Hossl, J., Hofestadt, J., Lefevre, D., Martinez-Mora, J. A., Nunez, A., Pavalas, G. E., Sanchez-Losa, A., Saldana, M., Schussler, F., Stolarczyk, T., Zniga, J., Arguelles, C., Tjus, J. B., Borner, M., Boser, S., De Andre, J. P. A. M., Diaz-Velez, J. C., Lorenzo, V. D., Glusenkamp, T., Hunnefeld, M., Kopke, L., Kruckl, G., Mariscal, C. J. L., Lunemann, J., Maris, I. C., Momente, G., Pollmann, A. O., De Los Heros, C. P., Herrera, S. E. S., Schoneberg, S., Stossl, A., Tonnis, C., Elorrieta, M. A. U., Arene, M., Becsy, B., Bustillo, J. C., Diaz, J. C., Cavaglia, M., Cerda-Duran, P., Cordero-Carrion, I., Canton, T. D., Dalya, G., Costa, C. F. D. S., Deleglise, S., Pozzo, W. D., Diaz, M. C., Girolamo, T. Di., Garcia-Quiros, C., Ghosh, A., Gonzalez, G., Castro, J. M. G., Kefelian, F., Kim, C., Krolak, A., Luck, H., Magana-Sandoval, F., Zertuche, L. 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Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Aix Marseille Université (AMU)-Institut de Recherche pour le Développement (IRD), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Collège de France (CdF)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), ESPCI ParisTech, Andre, M, Aubert, Jj, Barrios-Marti, J, Bouwhuis, Mc, Branzas, H, El Moursli, Rc, Coelho, Jab, Diaz, Af, Dona, R, Elsasser, D, Enzenhofer, A, Gregoire, T, Ruiz, Rg, van Haren, H, Heijboer, Aj, Hernandez-Rey, Jj, Hossl, J, Hofestadt, J, de Jong, M, Khan-Chowdhury, Nr, Lefevre, D, Martinez-Mora, Ja, Nunez, A, Pavalas, Ge, Sanchez-Losa, A, Saldana, M, Samtleben, Dfe, Schussler, F, Zornoza, Jd, Zuniga, J, Aartsen, Mg, Aguilar, Ja, Arguelles, C, Barron, Jp, Barwick, Sw, Beatty, Jj, Tjus, Jb, Becker, Kh, Besson, Dz, Borner, M, Boser, S, Bretz, Hp, Collin, Gh, Conrad, Jm, Cowen, Df, de Andre, Jpam, Delaunay, Jj, de Vries, Kd, de Wasseige, G, de With, M, Diaz-Velez, Jc, di Lorenzo, V, Dumm, Jp, Evenson, Pa, Fazely, Ar, Gaisser, Tk, Glusenkamp, T, Gonzalez, Jg, Hill, Gc, Hoffman, Kd, Hunnefeld, M, Jones, Bjp, Kelley, Jl, Klein, Sr, Kopke, L, Koschinsky, Jp, Koskinen, Dj, Kruckl, G, Lanfranchi, Jl, Larson, Mj, Liu, Qr, Mariscal, Cjl, Lunemann, J, Mahn, Kbm, Maris, Ic, Momente, G, Moore, Rw, Nowicki, Sc, Nygren, Dr, Pollmann, Ao, Pankova, Dv, Pepper, Ja, de los Heros, Cp, Price, Pb, Przybylski, Gt, Rea, Ic, Herrera, Se, Schoneberg, S, Spiczak, 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Mcclelland, De, Mcguire, Sc, Mcmanus, Dj, Mcwilliams, St, Meadors, Gd, Mehta, Ak, Mercer, Ra, Merilh, El, Meyers, Pm, Mikhailov, Ee, Miller, Al, Mills, Jc, Milovich-Goff, Mc, Mitrofanov, Vp, Mohapatra, Srp, Moore, Cj, Mow-Lowry, Cm, Muniz, Ea, Murray, Pg, Nayak, Rk, Nelson, Tjn, Ng, Ky, Nuttall, Lk, O'Brien, Bd, O'Dea, Gd, Ogin, Gh, Oh, Jj, Oh, Sh, Okada, Ma, Oram, Rj, Ormiston, Rg, Ortega, Lf, Ottaway, Dj, Owen, Bj, Pace, Ae, Page, Ma, Pai, Sa, Palamos, Jr, Pan, Hw, Pang, Pth, Pant, Bc, Pearlstone, Bl, Perez, Cj, Pfeiffer, Hp, Piccinni, Oj, Pong, Dyt, Porter, Ek, Prajapati, Ak, Prodi, Ga, Prokhorov, Lg, Purrer, M, Quinonez, Pj, Quintero, Ea, Raab, Fj, Ramirez, Ke, Reitze, Dh, Richardson, Cj, Richardson, Jw, Ricker, Pm, Robertson, Na, Rollins, Jg, Roma, Vj, Romel, Cl, Romie, Jh, Rosinska, D, Rosofsky, Sg, Ross, Mp, Rudiger, A, Sanchez, Ej, Sanchez, Le, Sanders, Jr, Santiago, Ka, Saulson, Pr, Savage, Rl, Schofield, Rm, Schonbeck, A, Schulte, Bw, Schutz, Bf, Schwalbe, Sg, Scott, Sm, Shaddock, Da, Shaner, Mb, Shoemaker, Dh, Shoemaker, Dm, Silva, Ad, Singer, Lp, Sintes, Am, Slagmolen, Bjj, Slaven-Blair, Tj, Smith, Jr, Smith, Rje, Son, Ej, Spencer, Ap, Srivastava, Ak, Steer, Da, Stevenson, Sp, Stops, Dj, Strain, Ka, Strigin, Se, Stuver, Al, Summerscales, Tz, Sutton, Pj, Swinkels, Bl, Szczepanczyk, Mj, Tait, Sc, Tanner, Db, Tapai, M, Tasson, Jd, Thondapu, Sr, Thorne, Ka, Torres-Forne, A, Torrie, Ci, Toyra, D, Tringali, Mc, Tsang, Kw, Urban, Al, Usman, Sa, van Bakel, N, van Beuzekom, M, van den Brand, Jfj, Van Den Broeck, C, Vander-Hyde, Dc, van der Schaaf, L, van Heijningen, Jv, van Veggel, Aa, Vasuth, M, Veitch, Pj, Vicere, A, Viets, Ad, Vine, Dj, Vinet, Jy, Vyatchanin, Sp, Wade, Ar, Wade, Le, Wang, Jz, Wang, Wh, Wang, Yf, Ward, Rl, Warden, Za, Wei, Lw, Weinstein, Aj, Wessel, Ek, Wessels, P, Westhouse, Jw, Whelan, Jt, Whiting, Bf, Wilken, Dm, Williamson, Ar, Willis, Jl, Wimmer, Mh, Wipf, Cc, Wofford, Jk, Wright, Jl, Wysocki, Dm, Yancey, Cc, Yap, Mj, Yeeles, Dw, Yu, Hc, Yuen, Shr, Zadrozny, Ak, Zendri, Jp, Zhu, Xj, Zucker, Me, Physics, Faculty of Sciences and Bioengineering Sciences, Vriendenkring VUB, Elementary Particle Physics, ITA, USA, GBR, FRA, DEU, ESP, Centre Tecnològic de Vilanova i la Geltrú, Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques, COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA), and Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS)
- Subjects
Astrofísica ,collapse [supernova] ,neutron star: binary ,EVENTS GW150914 ,Gravitació ,010504 meteorology & atmospheric sciences ,neutrino: energy: high ,Astronomy ,RAY ,Binary number ,binary [neutron star] ,Astrophysics ,7. Clean energy ,01 natural sciences ,Physical Chemistry ,Atomic ,IceCube ,neutrino ,Particle and Plasma Physics ,Astronomi, astrofysik och kosmologi ,black hole ,Astronomy, Astrophysics and Cosmology ,LIGO ,010303 astronomy & astrophysics ,gravitational wave ,ELECTROMAGNETIC SIGNALS ,QC ,QB ,Settore FIS/01 ,Physics ,High Energy Astrophysical Phenomena (astro-ph.HE) ,astro-ph.HE ,[PHYS]Physics [physics] ,Astrophysics::Instrumentation and Methods for Astrophysics ,neutrinos ,gravitational waves ,520 Astronomie und zugeordnete Wissenschaften ,ddc ,observatory ,Supernova ,astrophysics: density ,Physical Sciences ,Neutrino ,Astrophysics - High Energy Astrophysical Phenomena ,Astronomy and Astrophysics ,Space and Planetary Science ,Astronomical and Space Sciences ,signature ,Physical Chemistry (incl. Structural) ,supernova: collapse ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astronomy & Astrophysics ,Gravitational waves ,emission [gravitational radiation] ,Ones gravitacionals ,Coincident ,0103 physical sciences ,Gravitational Waves, Neutrinos, LIGO, Virgo, Antares, IceCube ,Nuclear ,ddc:530 ,Neutrins ,energy: high [neutrino] ,Neutrinos ,STFC ,Astrophysique ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences ,Science & Technology ,ANTARES ,Gravitational wave ,Virgo ,Organic Chemistry ,RCUK ,Molecular ,Astronomie ,Astronomy and Astrophysic ,530 Physik ,Sciences de l'espace ,Black hole ,messenger ,Neutron star ,Antares ,Physics and Astronomy ,FISICA APLICADA ,Física::Astronomia i astrofísica [Àrees temàtiques de la UPC] ,gravitational radiation: emission ,density [astrophysics] ,ddc:520 ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,EMISSION - Abstract
[EN] Astrophysical sources of gravitational waves, such as binary neutron star and black hole mergers or core-collapse supernovae, can drive relativistic outflows, giving rise to non-thermal high-energy emission. High-energy neutrinos are signatures of such outflows. The detection of gravitational waves and high-energy neutrinos from common sources could help establish the connection between the dynamics of the progenitor and the properties of the out¿ow. We searched for associated emission of gravitational waves and high-energy neutrinos from astrophysical transients with minimal assumptions using data from Advanced LIGO from its first observing run O1, and data from the ANTARES and IceCube neutrino observatories from the same time period. We focused on candidate events whose astrophysical origins could not be determined from a single messenger. We found no significant coincident candidate, which we used to constrain the rate density of astrophysical sources dependent on their gravitational-wave and neutrino emission processes., The ANTARES Collaboration acknowledge the financial support of the funding agencies: Centre National de la Recherche Scientifique (CNRS), Commissariat a l'energie atomique et aux energies alternatives (CEA), Commission Europeenne (FEDER fund and Marie Curie Program), Institut Universitaire de France (IUF), IdEx program and UnivEarthS Labex program at Sorbonne Paris Cite (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02), Labex OCEVU (ANR-11-LABX-0060) and the A*MIDEX project (ANR-11-IDEX-0001-02), Region Ile-de-France (DIM-ACAV), Region Alsace (contrat CPER), Region Provence-Alpes-Cote d'Azur, Departement du Var and Ville de La Seyne-sur-Mer, France; Bundesministerium fur Bildung und Forschung (BMBF), Germany; Istituto Nazionale di Fisica Nucleare (INFN), Italy; Nederlandse organisatie voor Wetenschappelijk Onderzoek (NWO), the Netherlands; Council of the President of the Russian Federation for young scientists and leading scientific schools supporting grants, Russia; National Authority for Scientific Research (ANCS), Romania; Ministerio de Economia y Competitividad (MINECO): Plan Estatal de Investigacion (refs. FPA2015-65150-C3-1-P, -2-P and -3-P, (MINECO/FEDER)), Severo Ochoa Centre of Excellence and MultiDark Consolider (MINECO), and Prometeo and Grisolia programs (Generalitat Valenciana), Spain; Ministry of Higher Education, Scientific Research and Professional Training, Morocco. We also acknowledge the technical support of Ifremer, AIM and Foselev Marine for the sea operation and the CC-IN2P3 for the computing facilities. The IceCube Collaboration gratefully acknowledges the following support: USA-U.S. National Science Foundation-Office of Polar Programs, U.S. National Science Foundation-Physics Division, Wisconsin Alumni Research Foundation, Center for High Throughput Computing (CHTC) at the University of Wisconsin-Madison, Open Science Grid (OSG), Extreme Science and Engineering Discovery Environment (XSEDE), U.S. Department of Energy-National Energy Research Scientific Computing Center, Particle astrophysics research computing center at the University of Maryland, Institute for Cyber-Enabled Research at Michigan State University, and Astroparticle physics computational facility at Marquette University; Belgium-Funds for Scientific Research (FRS-FNRS and FWO), FWO Odysseus and Big Science programmes, and Belgian Federal Science Policy Office (Belspo); Germany-Bundesministerium fur Bildung und Forschung (BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz Alliance for Astroparticle Physics (HAP), Initiative and Networking Fund of the Helmholtz Association, Deutsches Elektronen Synchrotron (DESY), and High Performance Computing cluster of the RWTH Aachen; Sweden-Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation; Australia-Australian Research Council; Canada-Natural Sciences and Engineering Research Council of Canada, Calcul Quebec, Compute Ontario, Canada Foundation for Innovation, WestGrid, and Compute Canada; Denmark-Villum Fonden, Danish National Research Foundation (DNRF); New Zealand-Marsden Fund; Japan-Japan Society for Promotion of Science (JSPS) and Institute for Global Prominent Research (IGPR) of Chiba University; Korea-National Research Foundation of Korea (NRF); Switzerland-Swiss National Science Foundation (SNSF). The LIGO Scientific Collaboration and the Virgo Collaboration gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council, etc.
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- 2019
13. Search for eccentric binary black hole mergers with advanced LIGO and advanced Virgo during their first and second observing runs
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Abbott, B. P, Abbott, R, Abbott, T. D, Abraham, S, Acernese, F, Ackley, K, Adams, C, Adhikari, R. X, Adya, V. B, Affeldt, C, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O. D, Aiello, L, Ain, A, Ajith, P, Allen, G, Allocca, A, Aloy, M. A, Altin, P. A, Amato, A, Anand, S, Ananyeva, A, Anderson, S. B, Anderson, W. G, Angelova, V, S, Antier, S, Appert, S, Arai, K, Araya, M. C, Areeda, J. S, Arene, M, Arnaud, N, Aronson, S. M, Arun, K. G, Ascenzi, S, Ashton, G, Aston, S. M, Astone, P, Aubin, F, Aufmuth, P, Aultoneal, K, Austin, C, Avendano, V and Avila-Alvarez, A, Babak, S, Bacon, P, Badaracco, F, Bader, M. K. M, Bae, S, Baird, J, Baker, P. T, Baldaccini, F, Ballardin, G, Ballmer, S. W, Bals, A, Banagiri, S, Barayoga, J. C, Barbieri, C, Barclay, S. E, Barish, B. C, Barker, D, Barkett, K, Barnum, S, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Bartos, I and Bassiri, R, Basti, A, Bawaj, M, Bayley, J. C, Bazzan, M, Bcsy, B, Bejger, M, Belahcene, I and Bell, A. 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Tasson, J, Taylor, R, Tenorio, R, Terkowski, L, Thomas, M, Thomas, P, Thondapu, S, Thorne, K, Thrane, E, Tiwari, S, Tiwari, V, Toland, K, Tonelli, M, Tornasi, Z, Torres-Forné, A, Torrie, C, Töyrä, D, Travasso, F, Traylor, G, Tringali, M, Tripathee, A, Trovato, A, Trozzo, L, Tsang, K, Tse, M, Tso, R, Tsukada, L, Tsuna, D, Tsutsui, T, Tuyenbayev, D, Ueno, K, Ugolini, D, Unnikrishnan, C, Urban, A, Usman, S, Vahlbruch, H, Vajente, G, Valdes, G, Valentini, M, Bakel, N, Beuzekom, M, Brand, J, Broeck, C, Vander-Hyde, D, Schaaf, L, Vanheijningen, J, Veggel, A, Vardaro, M, Varma, V, Vass, S, Vasúth, M, Vecchio, A, Vedovato, G, Veitch, J, Veitch, P, Venkateswara, K, Venugopalan, G, Verkindt, D, Vetrano, F, Viceré, A, Viets, A, Vinciguerra, S, Vine, D, Vinet, J, Vitale, S, Vo, T, Vocca, H, Vorvick, C, Vyatchanin, S, Wade, A, Wade, L, Wade, M, Walet, R, Walker, M, Wallace, L, Walsh, S, Wang, H, Wang, J, Wang, S, Wang, W, Wang, Y, Ward, R, Warden, Z, Warner, J, Was, M, Watchi, J, Weaver, B, Wei, L, Weinert, M, Weinstein, A, Weiss, R, Wellmann, F, Wen, L, Wessel, E, Weßels, P, Westhouse, J, Wette, K, Whelan, J, Whiting, B, Whittle, C, Wilken, D, Williams, D, Williamson, A, Willis, J, Willke, B, Winkler, W, Wipf, C, Wittel, H, Woan, G, Woehler, J, Wofford, J, Wright, J, Wu, D, Wysocki, D, Xiao, S, Xu, R, Yamamoto, H, Yancey, C, Yang, L, Yang, Y, Yang, Z, Yap, M, Yazback, M, Yeeles, D, Yu, H, Yuen, S, Zadrożny, A, Zanolin, M, Zelenova, T, Zendri, J, Zevin, M, Zhang, J, Zhang, L, Zhang, T, Zhao, C, Zhao, G, Zhou, M, Zhou, Z, Zhu, X, Zucker, M, Zweizig, J, Salemi, F, UCL - SST/IRMP - Institut de recherche en mathématique et physique, Laboratoire des matériaux avancés (LMA), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Kastler Brossel (LKB [Collège de France]), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF (institution))-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Lumière Matière [Villeurbanne] (ILM), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL), Institut de Physique Nucléaire de Lyon (IPNL), LIGO Scientific, Virgo, (Astro)-Particles Physics, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Collège de France (CdF (institution)), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), RS: FSE Grav. waves and fundamental physics, Grav. waves and fundamental physics, RS: FSE MSP, The LIGO Scientific Collaboration, The Virgo Collaboration, Arène, M., Bécsy, B., Bustillo, J. Calderón, Diaz, J. Casanueva, Cavaglià, M., Cerdá-Durán, P., Cieślar, M., Constancio Jr., M., Cordero-Carrión, I., Canton, T. Dal, Dálya, G., D’Angelo, B., D’Antonio, S., Costa, C. F. Da Silva, Laurentis, M. De, Deléglise, S., Pozzo, W. Del, Pietri, R. De, Rosa, R. De, Rossi, C. De, Varona, O. de, Díaz, M. C., Fiore, L. Di, Giorgio, C. Di, Giovanni, F. Di, Giovanni, M. Di, Girolamo, T. Di, Lieto, A. Di, Pace, S. Di, Palma, I. Di, Renzo, F. Di, Vivanco, Francisco Hernandez, Fronzè, G., García-Quirós, C., Ghosh, Abhirup, Ghosh, Archisman, González, G., Castro, J. M. Gonzalez, Gupta, Anchal, Hübner, M. T., Kéfélian, F., Kim, Chunglee, Krämer, C., Królak, A., Kumar, Rahul, Kumar, Rakesh, Lück, H., Hernandez, I. Magaña, Márka, S., Márka, Z., Villa, E. Mejuto, Mukherjee, Arunava, Mukherjee, Subroto, O’Brien, B. D., Oram, Richard J., O’Reilly, B., O’Shaughnessy, R., Périgois, C., Pürrer, M., Rana, Javed, Rosińska, D., Rüdiger, A., Schönbeck, A., Szczepańczyk, M. J., Tápai, M., Tiwari, Shubhanshu, Tiwari, Srishti, Torres-Forné, A., Töyrä, D., Bakel, N. van, Beuzekom, M. van, Brand, J. F. J. van den, Broeck, C. Van Den, Schaaf, L. van der, Veggel, A. A. van, Vasúth, M., Viceré, A., Weßels, P., Yu, Hang, Yu, Haocun, Zadrożny, A. K., Zadrożny, A., Abbott, Bp, Abbott, Td, Adhikari, Rx, Adya, Vb, Aguiar, Od, Aloy, Ma, Altin, Pa, Anderson, Sb, Anderson, Wg, Angelova, Sv, Araya, Mc, Arene, M, Aronson, Sm, Arun, Kg, Aston, Sm, Bader, Mkm, Baker, Pt, Ballmer, Sw, Barayoga, Jc, Barclay, Se, Barish, Bc, Bayley, Jc, Bcsy, B, Benjamin, Mg, Berry, Cpl, Bilenko, Ia, Bilgili, Sa, Bizouard, Ma, Blackburn, Jk, Blair, Cd, Blair, Dg, Blair, Rm, Boom, Ba, Brady, Pr, Brau, Je, Briggs, Jh, Brooks, Af, Brown, Dd, Bulten, Hj, Byer, Rl, Bustillo, Jc, Callister, Ta, Camp, Jb, Campbell, Wa, Cannon, Kc, Carney, Mf, Diaz, Jc, Cavaglia, M, Cerda-Duran, P, Chamberlin, Sj, Chase, Ea, Cheeseboro, Bd, Chen, Hy, Cheng, Hp, Cheong, Ck, Chia, Hy, Chung, Kw, Cieslar, M, Ciobanu, Aa, Clark, Ja, Cohadon, Pf, Collette, Cg, Cominsky, Lr, Constancio, M, Cooper, Sj, Corbitt, Tr, Cordero-Carrion, I, Corley, Kr, Costa, Ca, Coughlin, Mw, Coughlin, Sb, Coulon, Jp, Countryman, St, Covas, Pb, Cowan, Ee, Coward, Dm, Cowart, Mj, Coyne, Dc, Creighton, Jde, Creighton, Td, Crowder, Sg, Cullen, Tj, Canton, Tl, Dalya, G, D'Angelo, B, Danilishin, Sl, D'Antonio, S, Costa, Cf, Datrier, Leh, Daw, Ej, De Laurentis, M, Deleglise, S, Del Pozzo, W, Demarchi, Lm, De Pietri, R, De Rosa, R, De Rossi, C, de Varona, O, Diaz, Mc, Di Fiore, L, Di Giorgio, C, Di Giovanni, F, Di Giovanni, M, Di Girolamo, T, Di Lieto, A, Di Pace, S, Di Palma, I, Di Renzo, F, Divakarla, Ak, Dooley, Kl, Downes, Tp, Driggers, Jc, Ducoin, Jg, Dwyer, Se, Easter, Pj, Edo, Tb, Eisenstein, Ra, Essick, Rc, Etienne, Zb, Evans, Tm, Farr, Wm, Fauchon-Jones, Ej, Fejer, Mm, Ferreira, Ec, Ferreira, Ta, Fisher, Rp, Fishner, Jm, Font, Ja, Forsyth, Pwf, Fournier, Jd, Vivanco, Fh, Frolov, Vv, Fronze, G, Gabbard, Ha, Gadre, Bu, Gaebel, Sm, Gair, Jr, Gaonkar, Sg, Garcia-Quiros, C, Giaime, Ja, Giardina, Kd, Gibson, Dr, Gonzalez, G, Castro, Jmg, Gossan, Se, Green, Ac, Gretarsson, Em, Grimm, Sj, Guidi, Gm, Gulati, Hk, Gustafson, Ek, Hall, Br, Hall, Ed, Hamilton, Ez, Hanke, Mm, Hannam, Md, Hannuksela, Oa, Hansen, Tj, Harry, Gm, Harry, Iw, Hasskew, Rk, Haster, Cj, Hayes, Fj, Heintze, Mc, Holgado, Am, Holland, Na, Holz, De, Howell, Ej, Hoy, Cg, Hbner, Mt, Huerta, Ea, Huttner, Sh, Isa, Hn, Isac, Jm, Iyer, Br, Jadhav, Sj, Janthalur, Nn, Jenkins, Ac, Jones, Aw, Jones, Di, Jones, Jd, Jonker, Rjg, Kalaghatgi, Cv, Kanner, Jb, Kapadia, Sj, Keerthana, Nv, Kefelian, F, Khalili, Fy, Khazanov, Ea, Kim, Jc, Kim, Ym, King, Pj, Klika, Jh, Knowles, Td, Koehlenbeck, Sm, Korth, Wz, Kozak, Db, Kramer, C, Krolak, A, Lackey, Bd, Lai, Kh, Lam, Tl, Lane, Bb, Lang, Rn, Lanza, Rk, Lasky, Pd, Lecoeuche, Yk, Lee, Ch, Lee, Hk, Lee, Hm, Lee, Hw, Lenon, Ak, Li, Kjl, Li, Tgf, Linker, Sd, Littenberg, Tb, Lo, Rkl, London, Lt, Lough, Jd, Lousto, Co, Lower, Me, Luck, H, Lundgren, Ap, Macleod, Dm, Hernandez, Im, Magana-Sandoval, F, Magee, Rm, Mansell, Gl, Marka, S, Marka, Z, Martin, Iw, Martin, Rm, Martynov, Dv, Massinger, Tj, Mccann, Jj, Mcclelland, De, Mcguire, Sc, Mcmanus, Dj, Mcwilliams, St, Meadors, Gd, Mehta, Ak, Villa, Em, Mercer, Ra, Merilh, El, Meyers, Pm, Miller, Al, Mills, Jc, Milovich-Goff, Mc, Mitrofanov, Vp, Mohapatra, Srp, Moore, Cj, Mow-Lowry, Cm, Muiz, Ea, Murray, Pg, Nayak, Rk, Neil, Bf, Nelson, Tjn, Ng, Ky, Nichols, Sa, Nuttall, Lk, O'Brien, Bd, Ogin, Gh, Oh, Jj, Oh, Sh, Okada, Ma, Oram, Rj, O'Reilly, B, Ormiston, Rg, Ortega, Lf, O'Shaughnessy, R, Ottaway, Dj, Owen, Bj, Pace, Ae, Page, Ma, Pai, Sa, Palamos, Jr, Panda, Pk, Pang, Pth, Pant, Bc, Pearlstone, Bl, Pechsiri, Tc, Pedersen, Aj, Perez, Cj, Perigois, C, Pfeiffer, Hp, Piccinni, Oj, Pinto, Im, Pong, Dyt, Porter, Ek, Prajapati, Ak, Prodi, Ga, Purrer, M, Quinonez, Pj, Raab, Fj, Ramirez, Ke, Reitze, Dh, Richardson, Cj, Richardson, Jw, Ricker, Pm, Robertson, Na, Rollins, Jg, Roma, Vj, Romel, Cl, Romie, Jh, Rose, Ca, Rosinska, D, Rosofsky, Sg, Ross, Mp, Rudiger, A, Sanchez, Ej, Sanchez, Le, Sanders, Jr, Santiago, Ka, Savage, Rl, Schonabel, R, Schofield, Rm, Schnbeck, A, Schulte, Bw, Schutz, Bf, Scott, Sm, Shaddock, Da, Shaner, Mb, Shoemaker, Dh, Shoemaker, Dm, Singer, Lp, Sintes, Am, Slagmolen, Bjj, Slaven-Blair, Tj, Smith, Jr, Smith, Rje, Son, Ej, Spencer, Ap, Srivastava, Ak, Steer, Da, Stevenson, Sp, Stops, Dj, Strain, Ka, Strigin, Se, Stuver, Al, Summerscales, Tz, Sutton, Pj, Swinkels, Bl, Szczepanczyk, Mj, Tait, Sc, Tanner, Db, Tapai, M, Tasson, Jd, Thondapu, Sr, Thorne, Ka, Torres-Forne, A, Torrie, Ci, Toyra, D, Tringali, Mc, Tsang, Kw, Urban, Al, Usman, Sa, van Bakel, N, van Beuzekom, M, van den Brand, Jfj, Van Den Broeck, C, Vander-Hyde, Dc, van Der Schaaf, L, Vanheijningen, Jv, van Veggel, Aa, Vasuth, M, Veitch, Pj, Vicere, A, Viets, Ad, Vine, Dj, Vinet, Jy, Vyatchanin, Sp, Wade, Ar, Wade, Le, Wang, Jz, Wang, Wh, Wang, Yf, Ward, Rl, Warden, Za, Wei, Lw, Weinstein, Aj, Wessel, Ek, Wessels, P, Westhouse, Jw, Whelan, Jt, Whiting, Bf, Wilken, Dm, Williamson, Ar, Willis, Jl, Wipf, Cc, Wofford, Jk, Wright, Jl, Wysocki, Dm, Yancey, Cc, Yap, Mj, Yeeles, Dw, Yu, Hc, Yuen, Shr, Zadrozny, Ak, Zadrozny, A, Zendri, Jp, Zhu, Xj, and Zucker, Me
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Astrofísica ,Gravitació ,010504 meteorology & atmospheric sciences ,IMPACT ,Astronomy ,WAVES ,Binary number ,Astrophysics ,gravitational waves ,black hole ,LIGO ,Virgo ,LIGO-Virgo ,01 natural sciences ,Rendering (computer graphics) ,Gravitation ,Elliptical orbit ,COMPACT-OBJECT BINARIES ,Eccentric ,YOUNG STAR-CLUSTERS ,EVOLUTION ,PERTURBATIONS ,PROGENITORS ,Eccentricity (behavior) ,010303 astronomy & astrophysics ,orbit ,QC ,media_common ,QB ,Settore FIS/01 ,Physics ,High Energy Astrophysical Phenomena (astro-ph.HE) ,Astrophysical black holes ,Gravitational waves ,Elliptical orbits ,Justice and Strong Institutions ,Physical Sciences ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena ,Gravitational wave ,data analysis method ,SDG 16 - Peace ,media_common.quotation_subject ,Gravitational waves, Elliptical orbits, Astrophysical black holes ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astronomy & Astrophysics ,General Relativity and Quantum Cosmology ,Settore FIS/05 - Astronomia e Astrofisica ,Binary black hole ,binary: coalescence ,statistical analysis ,0103 physical sciences ,Waveform ,STFC ,0105 earth and related environmental sciences ,Science & Technology ,binary: formation ,SDG 16 - Peace, Justice and Strong Institutions ,gravitational radiation ,RCUK ,Astronomy and Astrophysics ,gravitational radiation detector ,detector: sensitivity ,VIRGO ,Physics and Astronomy ,black hole: binary ,Space and Planetary Science ,gravitational radiation: emission ,eccentric BBH ,star: mass ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] - Abstract
When formed through dynamical interactions, stellar-mass binary black holes may retain eccentric orbits ($e>0.1$ at 10 Hz) detectable by ground-based gravitational-wave detectors. Eccentricity can therefore be used to differentiate dynamically-formed binaries from isolated binary black hole mergers. Current template-based gravitational-wave searches do not use waveform models associated to eccentric orbits, rendering the search less efficient to eccentric binary systems. Here we present results of a search for binary black hole mergers that inspiral in eccentric orbits using data from the first and second observing runs (O1 and O2) of Advanced LIGO and Advanced Virgo. The search uses minimal assumptions on the morphology of the transient gravitational waveform. We show that it is sensitive to binary mergers with a detection range that is weakly dependent on eccentricity for all bound systems. Our search did not identify any new binary merger candidates. We interpret these results in light of eccentric binary formation models., 7 pages, 2 figures
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- 2019
14. Explosive Magnetotail Activity
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Joachim Birn, Joachim Raeder, Viacheslav Merkin, P. L. Pritchett, Yuri V. Khotyaintsev, Antonius Otto, Tetsuo Motoba, M. I. Sitnov, Evgeny Gordeev, Fulvia Pucci, Marco Velli, B. Ferdousi, Xu-Zhi Zhou, Andrei Runov, Evgeny V. Panov, and V. A. Sergeev
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Flapping motions ,Flux tube oscillations ,010504 meteorology & atmospheric sciences ,Whistler ,Particle acceleration ,Tearing instability ,Supra-arcade downflows ,Laboratory reconnection experiments ,interchange instability ,01 natural sciences ,Article ,Ballooning ,\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$B_{z}$\end{document}Bz hump ,Auroral beads ,Auroral beads/rays ,Current sheet ,Fusion, plasma och rymdfysik ,Astronomi, astrofysik och kosmologi ,Physics::Plasma Physics ,rays ,0103 physical sciences ,Astronomy, Astrophysics and Cosmology ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences ,Current sheet thinning ,Physics ,Flux tube ,Bursty bulk flows ,Plasma micro-instabilities ,Astronomy and Astrophysics ,Magnetic reconnection ,Plasma acceleration ,Fusion, Plasma and Space Physics ,Magnetic flux ,Computational physics ,Solar wind ,13. Climate action ,Space and Planetary Science ,Physics::Space Physics ,Dipolarization fronts ,hump ,Ballooning/interchange instability ,Magnetohydrodynamics ,Magnetotail - Abstract
Modes and manifestations of the explosive activity in the Earth’s magnetotail, as well as its onset mechanisms and key pre-onset conditions are reviewed. Two mechanisms for the generation of the pre-onset current sheet are discussed, namely magnetic flux addition to the tail lobes, or other high-latitude perturbations, and magnetic flux evacuation from the near-Earth tail associated with dayside reconnection. Reconnection onset may require stretching and thinning of the sheet down to electron scales. It may also start in thicker sheets in regions with a tailward gradient of the equatorial magnetic field \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$B_{z}$\end{document}Bz; in this case it begins as an ideal-MHD instability followed by the generation of bursty bulk flows and dipolarization fronts. Indeed, remote sensing and global MHD modeling show the formation of tail regions with increased \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$B_{z}$\end{document}Bz, prone to magnetic reconnection, ballooning/interchange and flapping instabilities. While interchange instability may also develop in such thicker sheets, it may grow more slowly compared to tearing and cause secondary reconnection locally in the dawn-dusk direction. Post-onset transients include bursty flows and dipolarization fronts, micro-instabilities of lower-hybrid-drift and whistler waves, as well as damped global flux tube oscillations in the near-Earth region. They convert the stretched tail magnetic field energy into bulk plasma acceleration and collisionless heating, excitation of a broad spectrum of plasma waves, and collisional dissipation in the ionosphere. Collisionless heating involves ion reflection from fronts, Fermi, betatron as well as other, non-adiabatic, mechanisms. Ionospheric manifestations of some of these magnetotail phenomena are discussed. Explosive plasma phenomena observed in the laboratory, the solar corona and solar wind are also discussed.
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- 2019
15. Magnetotail magnetic flux monitoring based on simultaneous solar wind and magnetotail observations
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Steve Milan, V. A. Sergeev, Evgeny Gordeev, Nikolai A. Tsyganenko, M. A. Shukhtina, and Lasse Boy Novock Clausen
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Physics ,010504 meteorology & atmospheric sciences ,Meteorology ,business.industry ,Geophysics ,ISTP ,01 natural sciences ,Magnetic flux ,Solar wind ,Space and Planetary Science ,Research council ,0103 physical sciences ,Data center ,Space Science ,business ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences - Abstract
This work was supported by Russian Science Foundation grant 14-17-00072. The CLUSTER-based tail magnetic flux computation for years 2001–2009 was supported by FP7 ECLAT project, they are now available via CSA. We are grateful to all teams for the opportunity to use their observational data. We thank NASA CDAWeb (http://cdaweb.gsfc.nasa.gov/istp_public/) for IMF, solar wind, and magnetic index data; the AMPERE project (http://ampere.jhuapl.edu) for AMPERE data; the THEMIS website (http://themis.ssl.berkeley.edu/) for THEMIS spacecraft data, Cluster Science Archive (http://www.cosmos.esa.int/web/csa) for Cluster data; the IMAGE-FUV data were supplied by the NASA Space Science Data Centre(NSSDC). The global MHD simulations were made possible due to NASA Community Coordinated Modeling Center effort (http://ccmc.gsfc.nasa.gov/). S.E.M. was supported by the Science and Technology Facilities Council (STFC), UK, grant ST/K001000/1. The work at the Birkeland Centre for Space Centre, University of Bergen, Norway, was supported by the Research Council of Norway/CoE under contract 223252/F50. We also thank Stepan Dubyagin for help in calculating THEMIS total pressure, Peter Boakes for data on magnetotail plasma domains, and Marianna Kholeva for help with the manuscript preparation.
- Published
- 2016
16. Modulation of the substorm current wedge by bursty bulk flows: 8 September 2002-Revisited
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Olaf Amm, V. A. Sergeev, Rumi Nakamura, Minna Palmroth, Kirsti Kauristie, Laurianne Palin, M. van de Kamp, T. Zivkovic, Alexander Nikolaev, Marina Kubyshkina, Gabor Facsko, Hermann Opgenoorth, Steve Milan, Suzanne M. Imber, and K. Ågren
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Physics ,010504 meteorology & atmospheric sciences ,Growth phase ,Magnetic signature ,Plasma ,Geophysics ,Expansion phase ,01 natural sciences ,Wedge (geometry) ,Space and Planetary Science ,0103 physical sciences ,Substorm ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences - Abstract
The ultimate formation mechanism of the substorm current wedge (SCW) remains to-date unclear. In this study, we investigate its relationship to plasma flows at substorm onset and throughout the following expansion phase. We revisit the case of September 8, 2002, which has been defined as "the best textbook example for a localized substorm onset observation" because of its excellent coverage by both spacecraft in the magnetotail and ground-based observatories is revisited. We found that a dense sequence of arrival of nightside flux transfer events (which can be understood as the lobe magnetic signature due to a bursty bulk flow travelling earthward in the central plasmasheet) in the near-Earth tail leads to a modulation (and further step-like built-up) of the SCW intensity during the substorm expansion phase. In addition, we found that small SCWs are created also during the growth phase of the event in association with another less intense sequence of NFTEs. The differences between the sequence of NFTEs in the growth and expansion phase are discussed. We conclude that the envelope of the magnetic disturbances which we typically refer to as an intense magnetic substorm is the result of a group or sequence of more intense and more frequent NFTEs.
- Published
- 2016
17. Magnetospheric conditions near the equatorial footpoints of proton isotropy boundaries
- Author
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Natalia Ganushkina, I. A. Chernyaev, Vassilis Angelopoulos, and V. A. Sergeev
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Physics ,Atmospheric Science ,Scattering ,Gyroradius ,Isotropy ,lcsh:QC801-809 ,Magnetosphere ,Geology ,Astronomy and Astrophysics ,Plasmasphere ,Geophysics ,Radius ,lcsh:QC1-999 ,Magnetic field ,Computational physics ,Current sheet ,lcsh:Geophysics. Cosmic physics ,Space and Planetary Science ,Physics::Space Physics ,Earth and Planetary Sciences (miscellaneous) ,lcsh:Q ,lcsh:Science ,lcsh:Physics - Abstract
Data from a cluster of three THEMIS (Time History of Events and Macroscale Interactions during Substorms) spacecraft during February–March 2009 frequently provide an opportunity to construct local data-adaptive magnetospheric models, which are suitable for the accurate mapping along the magnetic field lines at distances of 6–9 Re in the nightside magnetosphere. This allows us to map the isotropy boundaries (IBs) of 30 and 80 keV protons observed by low-altitude NOAA POES (Polar Orbiting Environmental Satellites) to the equatorial magnetosphere (to find the projected isotropy boundary, PIB) and study the magnetospheric conditions, particularly to evaluate the ratio KIB (Rc/rc; the magnetic field curvature radius to the particle gyroradius) in the neutral sheet at that point. Special care is taken to control the factors which influence the accuracy of the adaptive models and mapping. Data indicate that better accuracy of an adaptive model is achieved when the PIB distance from the closest spacecraft is as small as 1–2 Re. For this group of most accurate predictions, the spread of KIB values is still large (from 4 to 32), with the median value KIB ~13 being larger than the critical value Kcr ~ 8 expected at the inner boundary of nonadiabatic angular scattering in the current sheet. It appears that two different mechanisms may contribute to form the isotropy boundary. The group with K ~ [4,12] is most likely formed by current sheet scattering, whereas the group having KIB ~ [12,32] could be formed by the resonant scattering of low-energy protons by the electromagnetic ion-cyclotron (EMIC) waves. The energy dependence of the upper K limit and close proximity of the latter event to the plasmapause locations support this conclusion. We also discuss other reasons why the K ~ 8 criterion for isotropization may fail to work, as well as a possible relationship between the two scattering mechanisms.
- Published
- 2015
18. On the source region and orientations of nightside auroral arcs
- Author
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T. Bondareva, D. Gilles, Eric Donovan, and V. A. Sergeev
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Convection ,Physics ,Atmospheric Science ,010504 meteorology & atmospheric sciences ,Isotropy ,Equator ,Plasma sheet ,Magnetosphere ,Astrophysics ,Rotation ,01 natural sciences ,Current sheet ,Geophysics ,Space and Planetary Science ,Physics::Space Physics ,0103 physical sciences ,Ionosphere ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences - Abstract
Using large data base of stable auroral arcs observed at Gillam we identified those passes of POES spacecraft which were magnetically conjugate to these arcs. We studied statistically arc locations with respect to the energetic particle isotropy boundaries (IBs), which are the well-known markers of the magnetotail regions. In the dusk and night sectors we confirm previous finding that arcs tend to appear close to or poleward of the electron isotropy boundary (IBe), indicating the location of the arcs in the small BZ (large magnetic field curvature) region of the tail current sheet. Different from that, in the dawn sector significant fraction of arcs appears deeper in the magnetosphere, between electron and proton IBs, in the transition region between the current sheet and dipole-like magnetosphere. Addressing the orientations of stable arcs we use the empirical magnetospheric models to demonstrate that nearly sun-aligned plasma sheet structures in the tail are significantly rotated toward azimuthal alignment when mapped from the tail equator to the ionosphere. We discuss how the flow braking/rotation can provide (in direct or secondary/way) the E-W aligned arcs. Based on these results we argue that a significant fraction of the highlatitude stable auroral arcs could be formed by the fast flow convection channels (BBFs); particularly the observed dawn-dusk asymmetry in the relative location of arcs and isotropy boundary can be contributed by this mechanism.
- Published
- 2020
19. Energy–latitude dispersion patterns near the isotropy boundaries of energetic protons
- Author
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V. A. Sergeev, S. Apatenkov, Natalia Ganushkina, Stepan Dubyagin, and S. A. Chernyaeva
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Physics ,Atmospheric Science ,Proton ,Scattering ,Isotropy ,lcsh:QC801-809 ,Plasma sheet ,Magnetosphere ,Geology ,Astronomy and Astrophysics ,lcsh:QC1-999 ,Computational physics ,Current sheet ,lcsh:Geophysics. Cosmic physics ,Space and Planetary Science ,Physics::Space Physics ,Earth and Planetary Sciences (miscellaneous) ,Physics::Accelerator Physics ,lcsh:Q ,Ionosphere ,Atomic physics ,Dispersion (chemistry) ,lcsh:Science ,lcsh:Physics - Abstract
Non-adiabatic motion of plasma sheet protons causes pitch-angle scattering and isotropic precipitation to the ionosphere, which forms the proton auroral oval. This mechanism related to current sheet scattering (CSS) provides a specific energy–latitude dispersion pattern near the equatorward boundary of proton isotropic precipitation (isotropy boundary, IB), with precipitation sharply decreasing at higher (lower) latitude for protons with lower (higher) energy. However, this boundary maps to the inner magnetosphere, where wave-induced scattering may provide different dispersion patterns as recently demonstrated by Liang et al. (2014). Motivated by the potential usage of the IBs for the magnetotail monitoring as well as by the need to better understand the mechanisms forming the proton IB, we investigate statistically the details of particle flux patterns near the proton IB using NOAA-POES polar spacecraft observations made during September 2009. By comparing precipitated-to-trapped flux ratio (J0/J90) at >30 and >80 keV proton energies, we found a relatively small number of simple CSS-type dispersion events (only 31 %). The clear reversed (wave-induced) dispersion patterns were very rare (5 %). The most frequent pattern had nearly coinciding IBs at two energies (63 %). The structured precipitation with multiple IBs was very frequent (60 %), that is, with two or more significant J0/J90 dropouts. The average latitudinal width of multiple IB structures was about 1°. Investigation of dozens of paired auroral zone crossings of POES satellites showed that the IB pattern is stable on a timescale of less than 2 min (a few proton bounce periods) but can evolve on a longer (several minutes) scale, suggesting temporal changes in some mesoscale structures in the equatorial magnetosphere. We discuss the possible role of CSS-related and wave-induced mechanisms and their possible coupling to interpret the emerging complicated patterns of proton isotropy boundaries.
- Published
- 2018
20. Evaluation of the geometry of ionospheric current systems related to rapid geomagnetic variations
- Author
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Ari Viljanen, V. A. Sergeev, R. Pirjola, S. Apatenkov, and EGU, Publication
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Atmospheric Science ,Magnetosphere ,Geometry ,Physics::Geophysics ,Earth and Planetary Sciences (miscellaneous) ,lcsh:Science ,Ring current ,Physics ,[SDU.OCEAN] Sciences of the Universe [physics]/Ocean, Atmosphere ,lcsh:QC801-809 ,Geology ,Astronomy and Astrophysics ,Geophysics ,lcsh:QC1-999 ,Geomagnetically induced current ,Solar wind ,lcsh:Geophysics. Cosmic physics ,Amplitude ,Earth's magnetic field ,Space and Planetary Science ,Physics::Space Physics ,[SDU.STU] Sciences of the Universe [physics]/Earth Sciences ,Dynamic pressure ,lcsh:Q ,Ionosphere ,lcsh:Physics - Abstract
To learn about the geometry and sources of the ionospheric current systems which generate strong geomagnetically induced currents, we categorize differential equivalent current systems (DEC) for events with strong dB/dt by decomposing them into the contributions of electrojet-type and vortex-type elementary systems. By solving the inverse problem we obtain amplitudes and locations of these elementary current systems. One-minute differences of the geomagnetic field values at the IMAGE magnetometer network in 1996–2000 are analysed to study the spatial distributions of large dB/dt events. The relative contributions of the two components are evaluated. In particular, we found that the majority of the strongest dB/dt events (100–1000nT/min) appear to be produced by the vortex-type current structures and most of them occur in the morning LT hours, probably caused by the Ps6 pulsation events associated with auroral omega structures. For strong dB/dt events the solar wind parameters are shifted toward strong (tens nT) southward IMF, enhanced velocity and dynamic pressure, in order for the main phase of the magnetic storms to occur. Although these events appear mostly during magnetic storms when the auroral oval greatly expands, the area of large dB/dt stays in the middle part of the auroral zone; therefore, it is connected to the processes taking part in the middle of the magnetosphere rather than in its innermost region populated by the ring current. Key words. Geomagnetism and paleomagnetism (rapid time variations) – Ionosphere (auroral ionosphere; ionospheric disturbances)
- Published
- 2018
21. A quantitative study of magnetospheric magnetic field line deformation by a two-loop substorm current wedge
- Author
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Marina Kubyshkina, Howard J. Singer, Vassilis Angelopoulos, V. A. Sergeev, Hermann Opgenoorth, Alexander Nikolaev, and Nikolai A. Tsyganenko
- Subjects
Atmospheric Science ,Magnetospheric physics (auroral phenomena ,Wedge (geometry) ,Fusion, plasma och rymdfysik ,Substorm ,Earth and Planetary Sciences (miscellaneous) ,Geomagnetic latitude ,Surge ,lcsh:Science ,Physics ,lcsh:QC801-809 ,Plasma sheet ,Geology ,Astronomy and Astrophysics ,Geophysics ,current systems ,Fusion, Plasma and Space Physics ,lcsh:QC1-999 ,Magnetic field ,lcsh:Geophysics. Cosmic physics ,13. Climate action ,Space and Planetary Science ,Middle latitudes ,lcsh:Q ,Ionosphere ,storms and substorms) ,lcsh:Physics - Abstract
Substorm current wedge (SCW) formation is associated with global magnetic field reconfiguration during substorm expansion. We combine a two-loop model SCW (SCW2L) with a background magnetic field model to investigate distortion of the ionospheric footpoint pattern in response to changes of different SCW2L parameters. The SCW-related plasma sheet footprint shift results in formation of a pattern resembling an auroral bulge, the poleward expansion of which is controlled primarily by the total current in the region 1 sense current loop (I1). The magnitude of the footprint latitudinal shift may reach ∼ 10° corrected geomagnetic latitude (CGLat) during strong substorms (I1= 2 MA). A strong helical magnetic field around the field-aligned current generates a surge-like region with embedded spiral structures, associated with a westward traveling surge (WTS) at the western end of the SCW. The helical field may also contribute to rotation of the ionospheric projection of narrow plasma streams (auroral streamers). Other parameters, including the total current in the second (region 2 sense) loop, were found to be of secondary importance. Analyzing two consecutive dipolarizations on 17 March 2010, we used magnetic variation data obtained from a dense midlatitude ground network and several magnetospheric spacecraft, as well as the adaptive AM03 model, to specify SCW2L parameters, which allowed us to predict the magnitude of poleward auroral expansion. Auroral observations made during the two substorm activations demonstrate that the SCW2L combined with the AM03 model nicely describes the azimuthal progression and the observed magnitude of the auroral expansion. This finding indicates that the SCW-related distortions are responsible for much of the observed global development of bright auroras.
- Published
- 2018
22. Average characteristics of the midtail plasma sheet in different dynamic regimes of the magnetosphere
- Author
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N. P. Dmitrieva, M. A. Shukhtina, V. A. Sergeev, and EGU, Publication
- Subjects
Convection ,Atmospheric Science ,Flux ,Magnetosphere ,Substorm ,Earth and Planetary Sciences (miscellaneous) ,Astrophysics::Solar and Stellar Astrophysics ,lcsh:Science ,Physics ,[SDU.OCEAN] Sciences of the Universe [physics]/Ocean, Atmosphere ,lcsh:QC801-809 ,Plasma sheet ,Geology ,Astronomy and Astrophysics ,Geophysics ,Magnetic flux ,lcsh:QC1-999 ,Magnetic field ,Computational physics ,Solar wind ,lcsh:Geophysics. Cosmic physics ,Space and Planetary Science ,Physics::Space Physics ,[SDU.STU] Sciences of the Universe [physics]/Earth Sciences ,lcsh:Q ,lcsh:Physics - Abstract
We study average characteristics of plasma sheet convection in the middle tail during different magnetospheric states (Steady Magnetospheric Convection, SMC, and substorms) using simultaneous magnetotail (Geotail, 15-35 RE downtail) and solar wind (Wind spacecraft) observations during 3.5 years. (1) A large data set allowed us to obtain the average values of the plasma sheet magnetic flux transfer rate (Ey and directly compare it with the dayside transfer rate (Emod for different magnetospheric states. The results confirm the magnetic flux imbalance model suggested by Russell and McPherron(1973), namely: during SMC periods the day-to-night flux transport rate equals the global Earthward plasma sheet convection; during the substorm growth phase the plasma sheet convection is suppressed on the average by 40%, whereas during the substorm expansion phase it twice exceeds the day-to-night global flux transfer rate. (2) Different types of substorms were revealed. About 1/3 of all substorms considered displayed very weak growth in the tail lobe magnetic field before the onset. For these events the plasma sheet transport was found to be in a balance with the day-to-night flux transfer, as in the SMC events. However, the lobe magnetic field value in these cases was as large as that in the substorms with a classic growth phase just before the onset (both values exceed the average level of the lobe field during the SMC). Also, in both groups similar configurational changes (magnetic field stretching and plasma sheet thinning) were observed before the substorm onset. (3) Superimposed epoch analysis showed that the plasma sheet during the late substorm recovery phase has the characteristics similar to those found during SMC events, the SMC could be a natural magnetospheric state following the substorm.
- Published
- 2018
23. Global properties of magnetotail current sheet flapping: THEMIS perspectives
- Author
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Andrei Runov, V. A. Sergeev, Ian R. Mann, Vassilis Angelopoulos, Davin Larson, Uli Auster, J. P. McFadden, and Karl-Heinz Glassmeier
- Subjects
Physics ,Atmospheric Science ,Wave propagation ,Magnetometer ,lcsh:QC801-809 ,Plasma sheet ,Geology ,Astronomy and Astrophysics ,Geophysics ,lcsh:QC1-999 ,Magnetic field ,law.invention ,Computational physics ,Current sheet ,lcsh:Geophysics. Cosmic physics ,Amplitude ,Space and Planetary Science ,law ,Substorm ,Earth and Planetary Sciences (miscellaneous) ,Flapping ,lcsh:Q ,lcsh:Science ,lcsh:Physics - Abstract
A sequence of magnetic field oscillations with an amplitude of up to 30 nT and a time scale of 30 min was detected by four of the five THEMIS spacecraft in the magnetotail plasma sheet. The probes P1 and P2 were at X=−15.2 and −12.7 RE and P3 and P4 were at X=−7.9 RE. All four probes were at −6.5>Y>−7.5 RE (major conjunction). Multi-point timing analysis of the magnetic field variations shows that fronts of the oscillations propagated flankward (dawnward and Earthward) nearly perpendicular to the direction of the magnetic maximum variation (B1) at velocities of 20–30 km/s. These are typical characteristics of current sheet flapping motion. The observed anti-correlation between ∂B1/∂t and the Z-component of the bulk velocity make it possible to estimate a flapping amplitude of 1 to 3 RE. The cross-tail scale wave-length was found to be about 5 RE. Thus the flapping waves are steep tail-aligned structures with a lengthwise scale of >10 RE. The intermittent plasma motion with the cross-tail velocity component changing its sign, observed during flapping, indicates that the flapping waves were propagating through the ambient plasma. Simultaneous observations of the magnetic field variations by THEMIS ground-based magnetometers show that the flapping oscillations were observed during the growth phase of a substorm.
- Published
- 2018
24. Dayside isotropic precipitation of energetic protons
- Author
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G. R. Bikkuzina, V. A. Sergeev, Patrick T. Newell, Institute of Physics, Czech Academy of Sciences [Prague] (CAS), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), and EGU, Publication
- Subjects
Atmospheric Science ,010504 meteorology & atmospheric sciences ,Field line ,Magnetosphere ,[SDU.STU]Sciences of the Universe [physics]/Earth Sciences ,Noon ,01 natural sciences ,Physics::Geophysics ,Current sheet ,0103 physical sciences ,Earth and Planetary Sciences (miscellaneous) ,lcsh:Science ,010303 astronomy & astrophysics ,Physics::Atmospheric and Oceanic Physics ,0105 earth and related environmental sciences ,Physics ,[SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere ,Scattering ,[SDU.OCEAN] Sciences of the Universe [physics]/Ocean, Atmosphere ,Isotropy ,lcsh:QC801-809 ,Geology ,Astronomy and Astrophysics ,Geophysics ,lcsh:QC1-999 ,Computational physics ,Magnetic field ,lcsh:Geophysics. Cosmic physics ,13. Climate action ,Space and Planetary Science ,Physics::Space Physics ,[SDU.STU] Sciences of the Universe [physics]/Earth Sciences ,Magnetopause ,lcsh:Q ,Astrophysics::Earth and Planetary Astrophysics ,lcsh:Physics - Abstract
Recently it has been shown that isotropic precipitation of energetic protons on the nightside is caused by a non-adiabatic effect, namely pitch-angle scattering of protons in curved magnetic field lines of the tail current sheet. Here we address the origin of isotropic proton precipitation on the dayside. Computations of proton scattering regions in the magnetopheric models T87, T89 and T95 reveal two regions which contribute to the isotropic precipitation. The first is the region of weak magnetic field in the outer cusp which provides the 1–2° wide isotropic precipitation on closed field lines in a ~2–3 hour wide MLT sector centered on noon. A second zone is formed by the scattering on the closed field lines which cross the nightside equatorial region near the magnetopause which provides isotropic precipitation starting ≈ 1.5–2 h MLT from noon and which joins smoothly the precipitation coming from the tail current sheet. We also analyzed the isotropic proton precipitation using observations of NOAA low altitude polar spacecraft. We find that isotropic precipitation of >30 to >80 keV protons continues around noon forming the continuous oval-shaped region of isotropic precipitation. Part of this region lies on open field lines in the region of cusp-like or mantle precipitation, its equatorward part is observed on closed field lines. Near noon it extends ~1–2° below the sharp boundary of solar electron fluxes (proxy of the open/closed field line boundary) and equatorward of the cusp-like auroral precipitation. The observed energy dispersion of its equatorward boundary (isotropic boundary) agrees with model predictions of expected particle scattering in the regions of weak and highly curved magnetic field. We also found some disagreement with model computations. We did not observe the predicted split of the isotropic precipitation region into separate nightside and dayside isotropic zones. Also, the oval-like shape of the isotropic boundary has a symmetry line in 10–12 MLT sector, which with increasing activity rotates toward dawn while the latitude of isotropic boundary is decreasing. Our conclusion is that for both dayside and nightside the isotropic boundary location is basically controlled by the magnetospheric magnetic field, and therefore the isotropic boundaries can be used as a tool to probe the magnetospheric configuration in different external conditions and at different activity levels.
- Published
- 2018
25. Jets Downstream of Collisionless Shocks
- Author
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V. A. Sergeev, Daniel Schmid, S. H. Lee, Ferdinand Plaschke, Vadim Roytershteyn, Xochitl Blanco-Cano, Nojan Omidi, David G. Sibeck, Minna Palmroth, Tomas Karlsson, Martin Archer, P. Kajdič, and Heli Hietala
- Subjects
EARTHS BOW SHOCK ,010504 meteorology & atmospheric sciences ,Astrophysics::High Energy Astrophysical Phenomena ,AMPLITUDE MAGNETIC-STRUCTURES ,INNER PLASMA SHEET ,Magnetosphere ,Plasmoid ,MAGNETOSHEATH PLASMOIDS ,Astrophysics ,Astronomy & Astrophysics ,HOT FLOW ANOMALIES ,01 natural sciences ,Magnetosheath ,Jets ,0201 Astronomical and Space Sciences ,0103 physical sciences ,Coronal mass ejection ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences ,Physics ,Jet (fluid) ,Science & Technology ,Bow shock ,QUASI-PARALLEL SHOCKS ,Astronomy and Astrophysics ,BURSTY BULK FLOWS ,Foreshock ,Bow shocks in astrophysics ,LOW-FREQUENCY WAVES ,HIGH-SPEED JETS ,Solar wind ,Magnetopause ,13. Climate action ,Space and Planetary Science ,SOLAR-WIND ,Physical Sciences ,Physics::Space Physics - Abstract
The magnetosheath flow may take the form of large amplitude, yet spatially localized, transient increases in dynamic pressure, known as “magnetosheath jets” or “plasmoids” among other denominations. Here, we describe the present state of knowledge with respect to such jets, which are a very common phenomenon downstream of the quasi-parallel bow shock. We discuss their properties as determined by satellite observations (based on both case and statistical studies), their occurrence, their relation to solar wind and foreshock conditions, and their interaction with and impact on the magnetosphere. As carriers of plasma and corresponding momentum, energy, and magnetic flux, jets bear some similarities to bursty bulk flows, which they are compared to. Based on our knowledge of jets in the near Earth environment, we discuss the expectations for jets occurring in other planetary and astrophysical environments. We conclude with an outlook, in which a number of open questions are posed and future challenges in jet research are discussed.
- Published
- 2018
26. Formation of 30 KeV Proton Isotropic Boundaries During Geomagnetic Storms
- Author
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N. Yu. Ganushkina, V. A. Sergeev, and Stepan Dubyagin
- Subjects
Physics ,Geomagnetic storm ,Nuclear physics ,Geophysics ,010504 meteorology & atmospheric sciences ,Proton ,Space and Planetary Science ,0103 physical sciences ,Isotropy ,010303 astronomy & astrophysics ,01 natural sciences ,0105 earth and related environmental sciences - Published
- 2018
- Full Text
- View/download PDF
27. Three‐dimensional current systems and ionospheric effects associated with small dipolarization fronts
- Author
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Hermann Opgenoorth, C. Jacquey, V. A. Sergeev, Martin Connors, J-A Sauvaud, Lucile Turc, Geoffrey D. Reeves, Vassilis Angelopoulos, Laurianne Palin, Rumi Nakamura, and Howard J. Singer
- Subjects
Physics ,Solar wind ,Geophysics ,Amplitude ,Space and Planetary Science ,QUIET ,Substorm ,Plasma sheet ,Geosynchronous orbit ,Flux ,Ionosphere - Abstract
We present a case study of eight successive plasma sheet (PS) activations (usually referred to as bursty bulk flows or dipolarization fronts), associated with small individual B-ZGSM increases on 31 March 2009 (0200-0900 UT), observed by the Time History of Events and Macroscale Interactions During Substorms mission. This series of events happens during very quiet solar wind conditions, over a period of 7 h preceding a substorm onset at 1230 UT. The amplitude of the dipolarizations increases with time. The low-amplitude dipolarization fronts are associated with few (1 or 2) rapid flux transport events (RFT, E-h > 2 mV/m), whereas the large-amplitude ones encompass many more RFT events. All PS activations are associated with small and localized substorm current wedge (SCW)-like current system signatures, which seems to be the consequence of RFT arrival in the near tail. The associated ground magnetic perturbations affect a larger part of the contracted auroral oval when, in the magnetotail, more RFT are embedded in PS activations (> 5). Dipolarization fronts with very low amplitude, a type usually not included in statistical studies, are of particular interest because we found even those to be associated with clear small SCW-like current system and particle injections at geosynchronous orbit. This exceptional data set highlights the role of flow bursts in the magnetotail and leads to the conclusion that we may be observing the smallest form of a substorm or rather its smallest element. This study also highlights the gradual evolution of the ionospheric current disturbance as the plasma sheet is observed to heat up.
- Published
- 2015
28. Event study combining magnetospheric and ionospheric perspectives of the substorm current wedge modeling
- Author
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Juan V. Rodriguez, Nikolai A. Tsyganenko, Rumi Nakamura, Marina Kubyshkina, Howard J. Singer, Brian J. Anderson, Stephen E. Milan, John C. Coxon, Vassilis Angelopoulos, V. A. Sergeev, Haje Korth, and A. V. Nikolaev
- Subjects
Physics ,Geophysics ,Space and Planetary Science ,Middle latitudes ,Local time ,Physics::Space Physics ,Substorm ,Magnetosphere ,Ionosphere ,Ampere ,Wedge (geometry) ,Magnetic field - Abstract
Unprecedented spacecraft and instrumental coverage and the isolated nature and distinct step-like development of a substorm on 17 March 2010 has allowed validation of the two-loop substorm current wedge model (SCW2L). We find a close spatiotemporal relationship of the SCW with many other essential signatures of substorm activity in the magnetotail and demonstrate its azimuthally localized structure and stepwise expansion in the magnetotail. We confirm that ground SCW diagnostics makes it possible to reconstruct and organize the azimuthal spatiotemporal substorm development pattern with accuracy better than 1 h magnetic local time (MLT) in the case of medium-scale substorm. The Active Magnetosphere and Planetary Electrodynamics Response Experiment (AMPERE)-based study of global field-aligned current distribution indicates that (a) the SCW-related field-aligned current system consists of simultaneously activated R1- and R2-type currents, (b) their net currents have a R1-sense, and (c) locations of net current peaks are consistent with the SCW edge locations inferred from midlatitude variations. Thanks to good azimuthal coverage of four GOES and three Time History of Events and Macroscale Interactions during Substorms spacecraft, we evaluated the intensities of the SCW R1- and R2-like current loops (using the SCW2L model) obtained from combined magnetospheric and ground midlatitude magnetic observations and found the net currents consistent (within a factor of 2) with the AMPERE-based estimate. We also ran an adaptive magnetospheric model and show that SCW2L model outperforms it in predicting the magnetic configuration changes during substorm dipolarizations.
- Published
- 2014
29. Near-Earth plasma sheet boundary dynamics during substorm dipolarization
- Author
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Stephen A. Fuselier, Drew Turner, V. A. Sergeev, Robert J. Strangeway, Ferdinand Plaschke, Per-Arne Lindqvist, Rumi Nakamura, Howard J. Singer, Barbara Giles, Brian J. Anderson, A. Varsani, Barry Mauk, Guan Le, Joachim Birn, Daniel J. Gershman, Werner Magnes, Ian J. Cohen, Allison Jaynes, S. Apatenkov, Ken R. Bromund, Olivier Le Contel, David Fischer, Julia E. Stawarz, Christopher T. Russell, Robert E. Ergun, L. Kepko, Yuri V. Khotyaintsev, Tsugunobu Nagai, Anton Artemyev, James A. Slavin, Takuma Nakamura, Wolfgang Baumjohann, Laboratoire de Physique des Plasmas (LPP), Université Paris-Saclay-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-École polytechnique (X)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Southwest Research Institute [San Antonio] (SwRI), The University of Texas at San Antonio (UTSA), NASA Goddard Space Flight Center (GSFC), Royal Institute of Technology [Stockholm] (KTH ), Institute of Geophysics and Planetary Physics [Los Angeles] (IGPP), University of California [Los Angeles] (UCLA), and University of California-University of California
- Subjects
FRONTS ,Geochemistry & Geophysics ,010504 meteorology & atmospheric sciences ,FLOW ,lcsh:Geodesy ,Boundary (topology) ,01 natural sciences ,Mathematical Sciences ,AURORAL STREAMERS ,Astronomi, astrofysik och kosmologi ,[PHYS.PHYS.PHYS-PLASM-PH]Physics [physics]/Physics [physics]/Plasma Physics [physics.plasm-ph] ,Substorm ,Meteorology & Atmospheric Sciences ,Astronomy, Astrophysics and Cosmology ,Geosciences, Multidisciplinary ,010303 astronomy & astrophysics ,SATELLITE ,TAIL ,lcsh:QB275-343 ,02 Physical Sciences ,lcsh:QE1-996.5 ,Plasma sheet ,lcsh:Geography. Anthropology. Recreation ,Geology ,MAGNETOTAIL ,Magnetic field ,Field-aligned current ,Physical Sciences ,Physics::Space Physics ,Astrophysics::Earth and Planetary Astrophysics ,Earth (classical element) ,Plasma sheet boundary layer ,CURRENTS ,04 Earth Sciences ,RAPID FLUX TRANSPORT ,Physics::Geophysics ,0103 physical sciences ,01 Mathematical Sciences ,0105 earth and related environmental sciences ,Dipolarization ,Science & Technology ,Spacecraft ,business.industry ,Geophysics ,Frontier Letter ,SIMULATIONS ,EVOLUTION ,lcsh:Geology ,lcsh:G ,Space and Planetary Science ,Earth Sciences ,business ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] - Abstract
We report on the large-scale evolution of dipolarization in the near-Earth plasma sheet during an intense (AL ~ −1000 nT) substorm on August 10, 2016, when multiple spacecraft at radial distances between 4 and 15 R E were present in the night-side magnetosphere. This global dipolarization consisted of multiple short-timescale (a couple of minutes) B z disturbances detected by spacecraft distributed over 9 MLT, consistent with the large-scale substorm current wedge observed by ground-based magnetometers. The four spacecraft of the Magnetospheric Multiscale were located in the southern hemisphere plasma sheet and observed fast flow disturbances associated with this dipolarization. The high-time-resolution measurements from MMS enable us to detect the rapid motion of the field structures and flow disturbances separately. A distinct pattern of the flow and field disturbance near the plasma boundaries was found. We suggest that a vortex motion created around the localized flows resulted in another field-aligned current system at the off-equatorial side of the BBF-associated R1/R2 systems, as was predicted by the MHD simulation of a localized reconnection jet. The observations by GOES and Geotail, which were located in the opposite hemisphere and local time, support this view. We demonstrate that the processes of both Earthward flow braking and of accumulated magnetic flux evolving tailward also control the dynamics in the boundary region of the near-Earth plasma sheet.Graphical AbstractMultispacecraft observations of dipolarization (left panel). Magnetic field component normal to the current sheet (BZ) observed in the night side magnetosphere are plotted from post-midnight to premidnight region: a GOES 13, b Van Allen Probe-A, c GOES 14, d GOES 15, e MMS3, g Geotail, h Cluster 1, together with f a combined product of energy spectra of electrons from MMS1 and MMS3 and i auroral electrojet indices. Spacecraft location in the GSM X-Y plane (upper right panel). Colorcoded By disturbances around the reconnection jets from the MHD simulation of the reconnection by Birn and Hesse (1996) (lower right panel). MMS and GOES 14-15 observed disturbances similar to those at the location indicated by arrows Electronic supplementary material The online version of this article (doi:10.1186/s40623-017-0707-2) contains supplementary material, which is available to authorized users.
- Published
- 2017
30. On the increasing oscillation period of flows at the tailward retreating flux pileup region during dipolarization
- Author
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Marina Kubyshkina, Rumi Nakamura, Evgeny V. Panov, Vassilis Angelopoulos, V. A. Sergeev, A. A. Petrukovich, Wolfgang Baumjohann, and Karl-Heinz Glassmeier
- Subjects
Physics ,geography ,geography.geographical_feature_category ,Oscillation ,Plasma sheet ,Flux ,Geophysics ,Inlet ,Earth radius ,Time history ,Space and Planetary Science ,Flow oscillation ,Oscillatory flow - Abstract
On 23 March 2009 between 6:00 and 6:40 UT, three Time History of Events and Macroscale Interactions during Substorms probes (P3, P4, and P5) were at about −11.5 Earth radii (RE) and two (P1 and P2) were at −14 RE downtail. The inner probes (P3–P5) started to observe oscillatory flow braking with plasma sheet dipolarization due to flux pileup at about 6:04 UT. After 6:16 UT the flux pileup region (FPR) expanded tailward as the outer probes (P1 and P2) moved closer to the neutral sheet and began to observe oscillatory braking also. During the FPR tailward expansion, the flow oscillation period increased from about 3.5 min at P3–P5 to about 6.2 min at P1 and P2. Meanwhile, as observed by the all-sky camera at Rankin Inlet, auroral activity gradually moved northward indicating that the characteristics of oscillatory flows at the tailward retreating FPR may be crucial for understanding the magnetosphere-ionosphere coupling.
- Published
- 2014
31. Period and damping factor of P i 2 pulsations during oscillatory flow braking in the magnetotail
- Author
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Wolfgang Baumjohann, Marina Kubyshkina, Karl-Heinz Glassmeier, Rumi Nakamura, Vassilis Angelopoulos, V. A. Sergeev, Evgeny V. Panov, and A. A. Petrukovich
- Subjects
Physics ,Geophysics ,Period (periodic table) ,Space and Planetary Science ,Magnetometer ,law ,Plasma sheet ,Damping factor ,Ionosphere ,Oscillatory flow ,law.invention - Abstract
[2011] during the events to find THEMIS footprints. We next statistically comparethe period and damping factor of the plasma sheet oscillating flows with those of themagnetic pulsations at the conjugate ionospheric locations.Magnetotail observations were provided by the probes’ fluxgate magnetometers (FGM)[
- Published
- 2014
32. How to distinguish between kink and sausage modes in flapping oscillations?
- Author
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D. A. Sormakov, V. A. Sergeev, I. V. Kubyshkin, Daria Kubyshkina, Stepan Dubyagin, N. Yu. Ganushkina, Vladimir Semenov, and Nikolai V. Erkaev
- Subjects
Physics ,Current sheet ,Geophysics ,Amplitude ,Space and Planetary Science ,Physics::Space Physics ,Plasma sheet ,Magnetosphere ,Flapping ,Mechanics ,Magnetohydrodynamics ,Rotation ,Noise (radio) - Abstract
Flapping waves are most noticeable large-scale perturbations of the magnetotail current sheet, whose nature is still under discussion. They represent rather slow (an order of magnitude less than typical Alfven speed) waves propagating from the center of the sheet to its flanks with a typical speed of 20–60 km/s, amplitude of 1–2 Re and quasiperiod of 2–10 min. The double-gradient MHD model, which was elaborated in Erkaev et al. (2007) predicts two (kink and sausage) modes of the flapping waves with differences in their geometry and propagation velocity, but the mode structure is hard to resolve observationally. We investigate the possibility of mode identification by observing the rotation of magnetic field and plasma velocity vectors from a single spacecraft. We test theoretical results by analyzing the flapping oscillations observed by Time History of Events and Macroscale Interactions during Substorms spacecraft and confirm that character of observed rotation is consistent with kink mode determination made by using multispacecraft methods. Also, we checked how the existence of some obstructive conditions, such as noise, combined modes, and multiple sources of the flapping oscillations, can affect on the possibility of the modes separation with suggested method.
- Published
- 2014
33. Diamagnetic oscillations ahead of stopped dipolarization fronts
- Author
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Andrei Runov, Vassilis Angelopoulos, V. A. Sergeev, Karl-Heinz Glassmeier, and Howard J. Singer
- Subjects
Physics ,Plasma sheet ,Geosynchronous orbit ,Front (oceanography) ,Magnetosphere ,Geophysics ,Plasma ,Computational physics ,Earth's magnetic field ,Physics::Plasma Physics ,Space and Planetary Science ,Physics::Space Physics ,Geostationary orbit ,Longitudinal wave - Abstract
It is well established that fast flows in the magnetotail plasma sheet which are separated from the ambient plasma by dipolarization fronts brake in the tail-dipole transition region. Flow/front braking is suggested to play an important role in generation of compressional waves in the inner magnetosphere and geomagnetic pulsations. Because of the paucity of multipoint observations in the tail-dipole transition region, however, details of wave generation during flow/front braking are unknown. Using comprehensive coverage of the near-Earth plasma sheet and geostationary orbit by six spacecraft, we explore the relationship between dipolarization fronts that propagated earthward at x=−11 to −9RE and stopped at x=−9 to −8RE and compressional oscillations observed at x≈−8RE. The oscillations, which were diamagnetic (i.e., exhibited antiphase variations in magnetic and plasma pressures), were observed about a minute prior to front detection. The amplitude of the magnetic oscillations at −8RE was ∼5 nT; the wavelength was ∼0.5RE. Enhancements of magnetic oscillations with different frequencies and amplitudes of 1 to 2 and 2 to 4 nT were detected at geosynchronous orbit and on the ground, respectively. Analysis of observations reveals that although the fast flow/front stopped a few RE beyond geosynchronous orbit, the plasma compression propagated farther inward and excited compressional diamagnetic oscillations in the tail-dipole transition region.
- Published
- 2014
34. Testing a two-loop pattern of the substorm current wedge (SCW2L)
- Author
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Jian Yang, V. A. Sergeev, Howard J. Singer, Andrei Runov, Nikolai A. Tsyganenko, Alexander Nikolaev, and Vassilis Angelopoulos
- Subjects
Physics ,Geophysics ,Amplitude ,Space and Planetary Science ,Middle latitudes ,Substorm ,Model parameters ,Geodesy ,Wedge (geometry) ,Current loop ,Magnetic field ,Computational physics - Abstract
Recent quantitative testing of the classical (region 1 sense) substorm current wedge (SCI) model revealed systematic discrepancies between the observed and predicted amplitudes, which suggested us to include additional region 2 sense currents (R2 loop) earthward of the dipolarized region (SCW2L model). Here we discuss alternative circuit geometries of the 3-D substorm current system and interpret observations of the magnetic field dipolarizations made between 6.6RE and 11RE, to quantitatively investigate the SCW2L model parameters. During two cases of a dipole-like magnetotail configuration, the dipolarization/injection front fortuitously stopped at r ~ 9RE for the entire duration of ~ 30 min long SCW-related dipolarization within a unique, radially distributed multispacecraft constellation, which allowed us to determine the locations and total currents of both SCW2L loops. In addition, we analyzed the dipolarization amplitudes in events, simultaneously observed at 6.6RE, 11RE and at colatitudes under a wide range of magnetograph conditions. We infer that the ratio I2/I1 varies in the range 0.2 to 0.6 (median value 0.4) and that the equatorial part of the R2 current loop stays at r>6.6RE in the case of a dipole-like field geometry (BZ0>75 nT at 6.6RE prior to the onset), but it is located at r
- Published
- 2014
35. Verification of the GUMICS-4 global MHD code using empirical relationships
- Author
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Evgeny Gordeev, Pekka Janhunen, Gabor Facsko, V. A. Sergeev, S. Milan, Minna Palmroth, and Ilja Honkonen
- Subjects
Physics ,010504 meteorology & atmospheric sciences ,Plasma sheet ,Magnetosphere ,Space physics ,Geophysics ,01 natural sciences ,Computational physics ,Solar wind ,Space and Planetary Science ,Physics::Space Physics ,0103 physical sciences ,Magnetopause ,Interplanetary magnetic field ,Magnetohydrodynamics ,Ionosphere ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences - Abstract
[1] Global magnetohydrodynamic (MHD) modeling is a powerful tool in space physics research. There are several advanced and still developing global MHD codes that are widely used to simulate plasma processes in solar wind magnetosphere-ionosphere system. The verification of global simulation codes is an important but a difficult problem. We present an approach for systematic and quantitative testing of code performance based on statistical empirical dependencies of the key magnetospheric parameters obtained from observations. We demonstrate the applicability of the method by testing the Grand Unified Magnetosphere Ionosphere Coupling simulation (GUMICS-4) global MHD model. A large set of nearly stationary solutions (162 runs altogether) with different stationary interplanetary magnetic field (IMF) and solar wind inputs were generated for different dipole tilts and levels of solar EUV radiation. As key parameters, we use the large-scale characteristics of the magnetosphere, including the magnetopause size and shape, geometry of the tail neutral sheet, magnetotail plasma pressure, tail lobe magnetic field, and cross-polar cap electric potential. We found that the GUMICS-4 stationary solutions generally fit the statistical relations, however, with some discrepancies. Particularly, position of the subsolar magnetopause, neutral sheet shape and position, and the plasma sheet pressure during northward IMF agree well with statistical models. At the same time, the size of the tail magnetopause and the lobe magnetic field magnitude appear to be systematically lower compared to their empirical values. Furthermore, the ionospheric potential is smaller in magnitude compared to empirical relations. These results provide an important starting point in the further development of the GUMICS simulation.
- Published
- 2013
36. Ionospheric response to oscillatory flow braking in the magnetotail
- Author
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Karl-Heinz Glassmeier, Olaf Amm, Evgeny V. Panov, Rumi Nakamura, A. A. Petrukovich, V. A. Sergeev, Marina Kubyshkina, James M. Weygand, Wolfgang Baumjohann, and Vassilis Angelopoulos
- Subjects
Physics ,010504 meteorology & atmospheric sciences ,Magnetometer ,Plasma sheet ,Magnetosphere ,Conductance ,Geophysics ,Polarization (waves) ,01 natural sciences ,Computational physics ,law.invention ,13. Climate action ,Space and Planetary Science ,law ,Physics::Space Physics ,0103 physical sciences ,Substorm ,Ionosphere ,010303 astronomy & astrophysics ,Pressure gradient ,0105 earth and related environmental sciences - Abstract
[1] We study the ionospheric response to oscillatory braking of bursty bulk flow observed by THEMIS on 17 March 2008 between 10:22 and 10:36 UT. By calculating different current components generated in the plasma sheet and correlating the space and ground observations, we discriminate the ionospheric current relevant to the large-scale substorm wedge currents produced by the general reconfiguration of the magnetotail pressure gradient from the currents that appeared as a result of the flow oscillation. While the former currents are large and quasi-stable, the latter (oscillating) currents are substantially (2–3 times) weaker and flow in opposite directions during earthward and tailward flow bursts. The oscillating currents include the polarization current and the current generated by the oscillating part of the pressure gradient. The two oscillating currents appear to produce modulation of the ionospheric currents (with about 2.5 min period) that was seen as Pi2 pulsations in the ground magnetometer observations. Our estimates of the ionospheric conductance suggest that the damping of the plasma sheet flow oscillation is due to heating the ionosphere through Pedersen currents. We also found that the all-sky imager at Fort Yukon observed four auroral forms during the first two periods of the oscillatory flow braking: two auroral forms related to the earthward plasma sheet flows and the other two auroral forms related to the tailward rebounds of the earthward flow. The auroral forms evolve in accordance with the appearance and motion of the upward field-aligned current spot of the modulated part of the ionospheric field-aligned current.
- Published
- 2013
37. Dipolarization fronts in the magnetotail plasma sheet
- Author
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Rumi Nakamura, Martin Connors, Harald U. Frey, U. Auster, Andrei Runov, J. P. McFadden, Davin Larson, Yukitoshi Nishimura, John W. Bonnell, V. A. Sergeev, M. I. Sitnov, Karl-Heinz Glassmeier, Vassilis Angelopoulos, Christopher T. Russell, and Howard J. Singer
- Subjects
Physics ,Leading edge ,Electron density ,Gyroradius ,Plasma sheet ,Astronomy and Astrophysics ,Geophysics ,Plasma ,Ion ,Physics::Plasma Physics ,Space and Planetary Science ,Physics::Space Physics ,Thermal ,Astrophysical plasma - Abstract
We present a THEMIS study of a dipolarization front associated with a bursty bulk flow (BBF) that was observed in the central plasma sheet sequentially at X=−20.1, −16.7, and −11.0RE. Simultaneously, the THEMIS ground network observed the formation of a north–south auroral form and intensification of westward auroral zone currents. Timing of the signatures in space suggests earthward propagation of the front at a velocity of 300 km/s. Spatial profiles of current and electron density on the front reveal a spatial scale of 500 km, comparable to an ion inertial length and an ion thermal gyroradius. This kinetic-scale structure traveled a macroscale distance of 10RE in about 4 min without loss of coherence. The dipolarization front, therefore, is an example of space plasma cross-scale coupling. THEMIS observations at different geocentric distances are similar to recent particle-in-cell simulations demonstrating the appearance of dipolarization fronts on the leading edge of plasma fast flows in the vicinity of a reconnection site. Dipolarization fronts, therefore, may be interpreted as remote signatures of transient reconnection.
- Published
- 2011
38. Comparison of magnetotail magnetic flux estimates based on global auroral images and simultaneous solar wind—magnetotail measurements
- Author
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A. D. DeJong, M. A. Shukhtina, V. A. Sergeev, and Benoît Hubert
- Subjects
Physics ,Atmospheric Science ,Correlation coefficient ,Proton ,Magnetosphere ,Geophysics ,Magnetic flux ,Computational physics ,Solar wind ,Space and Planetary Science ,Electric field ,Linear regression ,Substorm - Abstract
We compared simultaneous magnetotail magnetic flux F estimates, (1) based on in situ spacecraft measurements in the tail and solar wind (FT) with (2) the polar cap magnetic flux, estimated from global auroral images (using proton-induced or electron-induced emissions, Fp or Fe, respectively). Simultaneous Fp and Fe estimates gave the correlation coefficient CC=0.74, indicating that these measures are not absolutely precise. Regression analysis of FT versus Fe and Fp gave CC values 0.73 and 0.50, correspondingly. FT values, containing closed magnetic flux, are systematically higher than Fp and Fe by 20–30%. Motivated by diverse results, published by different groups, we reanalyzed the F dependence on the dayside merging electric field Em for different dynamical states. The linear regression F(Em) for substorm onsets shows a large slope ∼ 0.07 – 0.12 GWb / ( mV / m ) for all Fp, Fe and FT, confirming the loading–unloading substorm scheme. For SMC intervals this slope is only 0.03 GWb/(mV/m).
- Published
- 2010
39. Radial propagation velocity of energetic particle injections according to measurements onboard the Cluster satellites
- Author
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Rumi Nakamura, S. Apatenkov, M. A. Shukhtina, V. A. Sergeev, P. W. Daly, T. M. Sugak, and Wolfgang Baumjohann
- Subjects
Physics ,Space and Planetary Science ,Physics::Space Physics ,Substorm ,Aerospace Engineering ,Magnetosphere ,Astronomy and Astrophysics ,Geophysics ,Electron ,Plasma ,Computational physics - Abstract
Injections of energetic electrons with a dispersion over energies were observed during the February 23, 2004 (at about 03:20 UT) substorm onboard the Cluster satellites in the vicinity of perigee near the midnight meridian. The delays in the particle observation caused by the energy dependence of the magnetic drift velocities made it possible to determine the position and time of the beginning of the drift, tracing the trajectories of the leading center of particles back in time in the magnetospheric model. The comparisons of the measurements of four satellites allowed us to determine the radial propagation of the injection front with a velocity of 100–150 km/s at a distance of 7–9 RE. The comparison with a few previous measurements shows a substantial slowing down of injections as they approached the Earth, and this confirms the prospects of this method for more detailed study of propagation of plasma injection into the inner magnetosphere.
- Published
- 2009
40. Ionospheric signatures during a magnetospheric flux rope event
- Author
-
Kirsti Kauristie, Harald U. Frey, Rumi Nakamura, Olaf Amm, James A. Slavin, V. A. Sergeev, Christopher J. Owen, Liisa Juusola, and Andrew Walsh
- Subjects
Physics ,Atmospheric Science ,lcsh:QC801-809 ,Plasma sheet ,Flux ,Magnetosphere ,Geology ,Astronomy and Astrophysics ,Geophysics ,lcsh:QC1-999 ,lcsh:Geophysics. Cosmic physics ,Space and Planetary Science ,Substorm ,Physics::Space Physics ,Earth and Planetary Sciences (miscellaneous) ,Satellite ,Ionospheric heater ,lcsh:Q ,Ionosphere ,lcsh:Science ,lcsh:Physics ,Rope - Abstract
On 13 August 2002, during a substorm, Cluster encountered two earthward moving flux ropes (FR) in the central magnetotail. The first FR was observed during the expansion phase of the substorm, and the second FR during the recovery phase. In the conjugate ionospheric region in Northern Fennoscandia, the ionospheric equivalent currents were observed by the MIRACLE network and the auroral evolution was monitored by the Wideband Imaging Camera (WIC) on-board the IMAGE satellite. Extending the study of Amm et al. (2006), we examine and compare the possible ionospheric signatures associated with the two FRs. Amm et al. studied the first event in detail and found that the ionospheric footprint of Cluster coincided with a region of downward field-aligned current. They suggested that this region of downward current, together with a trailing region of upward current further southwestward, might correspond to the ends of the FR. Unlike during the first FR, however, we do not see any clear ionospheric features associated with the second one. In the GSM xy-plane, the first flux rope axis was tilted with respect to the y-direction by 29°, while the second flux rope axis was almost aligned in the y-direction, with an angle of 4° only. It is possible that due to the length and orientation of the second FR, any ionospheric signatures were simply mapped outside the region covered by the ground-based instruments. We suggest that the ground signatures of a FR depend on the orientation and the length of the structure.
- Published
- 2008
41. Topology of magnetic flux ropes in the magnetospheric plasma sheet as measured by the Geotail spacecraft
- Author
-
V. A. Sergeev and D. A. Sormakov
- Subjects
Physics ,Aerospace Engineering ,Astronomy and Astrophysics ,Magnetic reconnection ,Geophysics ,Magnetic flux ,Computational physics ,L-shell ,Space and Planetary Science ,Magnetic cloud ,Interplanetary magnetic field ,Mercury's magnetic field ,Topology (chemistry) ,Magnetosphere particle motion - Published
- 2008
42. Conjugate observation of sharp dynamical boundary in the inner magnetosphere by Cluster and DMSP spacecraft and ground network
- Author
-
F. Rich, Yu. Chotyaintsev, Rumi Nakamura, Andrei Runov, Andrew Fazakerley, I. Alexeev, Olaf Amm, J. A. Sauvaud, Wolfgang Baumjohann, S. Apatenkov, V. A. Sergeev, and P. W. Daly
- Subjects
Physics ,Atmospheric Science ,Field line ,lcsh:QC801-809 ,Plasma sheet ,Boundary (topology) ,Magnetosphere ,Geology ,Astronomy and Astrophysics ,Geophysics ,Astrophysics ,lcsh:QC1-999 ,Relativistic particle ,lcsh:Geophysics. Cosmic physics ,Boundary layer ,Space and Planetary Science ,Earth and Planetary Sciences (miscellaneous) ,Cluster (physics) ,Magnetopause ,lcsh:Q ,lcsh:Science ,lcsh:Physics - Abstract
We investigate an unusual sharp boundary separating two plasma populations (inner magnetospheric plasma with high fluxes of energetic particles and plasma sheet) observed by the Cluster quartet near its perigee on 16 December 2003. Cluster was in a pearl-on-string configuration at 05:00 MLT and mapped along magnetic field lines to ~8–9 RE in the equatorial plane. It was conjugate to the MIRACLE network and the DMSP F16 spacecraft passed close to Cluster footpoint. The properties of the sharp boundary, repeatedly crossed 7 times by five spacecraft during ~10 min, are: (1) upward FAC sheet at the boundary with ~30 nA/m2 current density at Cluster and ~2000 nA/m2 at DMSP; (2) the boundary had an embedded layered structure with different thickness scales, the electron population transition was at ~20 km scale at Cluster (
- Published
- 2008
43. Dynamical response of the magnetotail to changes of the solar wind direction: an MHD modeling perspective
- Author
-
V. A. Sergeev, Nikolai A. Tsyganenko, and Vassilis Angelopoulos
- Subjects
Physics ,Atmospheric Science ,Wave propagation ,lcsh:QC801-809 ,Magnetosphere ,Geology ,Astronomy and Astrophysics ,Mechanics ,Geophysics ,Classification of discontinuities ,lcsh:QC1-999 ,Discontinuity (linguistics) ,Solar wind ,lcsh:Geophysics. Cosmic physics ,Space and Planetary Science ,Substorm ,Earth and Planetary Sciences (miscellaneous) ,lcsh:Q ,Total pressure ,Magnetohydrodynamics ,lcsh:Science ,lcsh:Physics - Abstract
We performed global MHD simulations to investigate the magnetotail response to the solar wind directional changes (Vz-variations). These changes, although small, cause significant variations of the neutral sheet shape and location even in the near and middle tail regions. They display a complicated temporal response, in which ~60 to 80% of the final shift of the neutral sheet in Z direction occurs within first 10–15 min (less for faster solar wind), whereas a much longer time (exceeding half hour) is required to reach a new equilibrium. The asymptotic equilibrium shape of the simulated neutral sheet is consistent with predictions of Tsyganenko-Fairfield (2004) empirical model. To visualize a physical origin of the north-south tail motion we compared the values of the total pressure in the northern and southern tail lobes and found a considerable difference (10–15% for only 6° change of the solar wind direction used in the simulation). That difference builds up during the passage of the solar wind directional discontinuity and is responsible for the vertical shift of the neutral sheet, although some pressure difference remains in the near tail even near the new equilibrium. Surprisingly, at a given tailward distance, the response was found to be first initiated in the tail center (the "leader effect"), rather than near the flanks, which can be explained by the wave propagation in the tail, and which may have interesting implications for the substorm triggering studies. The present results have serious implications for the data-based modeling, as they place constraints on the accuracy of tail magnetic configurations to be derived for specific events using data of multi-spacecraft missions, e.g. such as THEMIS.
- Published
- 2008
44. On the plasma sheet dependence on solar wind and substorms and its role in magnetosphere-ionosphere coupling
- Author
-
Andrei Runov, N. P. Dmitrieva, V. A. Sergeev, N. A. Stepanov, Vassilis Angelopoulos, and D. A. Sormakov
- Subjects
Physics ,Plasma sheet ,Magnetosphere ,Geology ,Geophysics ,Plasma acceleration ,Particle acceleration ,Solar wind ,Space and Planetary Science ,Physics::Space Physics ,Substorm ,Electron temperature ,Atomic physics ,Ionosphere - Abstract
Recently, it was argued that Hall conductivity and peak intensity of equivalent ionospheric currents are sensitive to the amount of field-aligned acceleration of plasma sheet (PS) electrons, which in turn depends on the plasma sheet parameters T e and N e (electron temperature and density) proportionally to the quantity eTN = (T e)1/2/N e. Here we extend these studies using data from six tail seasons of THEMIS observations to show statistically that the behavior of these PS electron parameters, measured in the middle of the nightside plasma sheet at ~10 RE distance, depends in a very different way on two basic processes: the solar wind state and substorms. We confirm previous work that slow/dense (fast/tenuous) solar wind provides cold/dense (hot/tenuous) plasma sheet conditions. However, we find that electron temperature and pressure parameters (T e and P e) behave differently from the proton ones (T p and P p), indicating a strong decoupling between temperature variations of auroral protons and electrons in the central plasma sheet (CPS): electrons are more sensitive to the substorm-related acceleration in the magnetotail than protons. Our superposed epoch study of plasma sheet parameter variations during substorms as well as our analysis of plasma acceleration at dipolarization fronts shows that during the substorm expansion phase a new (accelerated and plasma-depleted) population comes into the inner CPS with the flow bursts, showing an average increase of electron temperature and eTN parameter roughly by a factor of 2 above its background values for both cold/dense and hot/tenuous plasma sheet states. Preferential electron heating in the flow bursts is also statistically confirmed.
- Published
- 2015
45. Association of Pi2 pulsations and pulsed reconnection: ground and Cluster observations in the tail lobe at 16 RE
- Author
-
Olaf Amm, H. Rème, V. A. Sergeev, E. A. Lucek, A. Keiling, Hiroshi Hasegawa, Masaki Fujimoto, I. Dandouras, Vladimir Semenov, Farideh Honary, and Harald U. Frey
- Subjects
Physics ,Atmospheric Science ,010504 meteorology & atmospheric sciences ,Electrojet ,Magnetosphere ,Geology ,Astronomy and Astrophysics ,Geophysics ,Polarization (waves) ,01 natural sciences ,Latitude ,13. Climate action ,Space and Planetary Science ,Middle latitudes ,Physics::Space Physics ,0103 physical sciences ,Substorm ,Earth and Planetary Sciences (miscellaneous) ,Astrophysics::Solar and Stellar Astrophysics ,Flux transfer event ,Ionosphere ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences - Abstract
Simultaneous measurements from the Cluster spacecraft and several ground stations (SAMNET, IMAGE, Kakioka, Hermanus) provide evidence for an association of Pi2 pulsations and pulsed reconnection in the magnetotail. On 8 September 2002, substorm-related Pi2 pulsations were recorded with the same waveform (same frequency) in the tail lobe at 16 RE and time-delayed on the ground (both nightside and dayside) spanning L values from 1.23 to 6.11. The tail lobe Pi2 pulsations were a series of nightside flux transfer event (NFTE) pulses propagating at a speed of 600–800 km/s towards Earth, which for the first time relates these two magnetospheric phenomena. NFTEs have previously been considered as the remote signature of tail reconnection. The first ground onset of the Pi2 pulsations occurred at high- and midlatitude ground stations with a time delay of ~30 s with respect to the tail lobe Pi2, followed by lower latitude ground stations. The largest pulsations were observed at high latitude (ten times larger than at low latitude) near the polar cap boundary. The polarization pattern of the ground Pi2s in the H-D plane was consistent with a periodically driven field-aligned current (FAC) system. In addition, fast mode waves must have also played a role in the inner magnetosphere because of propagation effects among ground stations and because of the simultaneous occurrence of dayside low-latitude Pi2. Auroral brightening occurred in the region of upflowing FAC, and the auroral electrojet expanded poleward together with the auroral bulge both of which are typical substorm signatures. Hence, we conclude that the substorm-related Pi2 pulsations in space at 16 RE and on the ground were remotely driven by pulsed reconnection in the magnetotail, that is, reconnection not only provided the energy but its temporal variations also determined the characteristic Pi2 frequency. Scenarios are discussed that address the connection of pulsed reconnection and the driven current system in the ionosphere. These results show that reconnection can be coupled to the ionosphere through what is phenomenologically known as Pi2 pulsations. As a corollary, it is shown that the time history of events fits within the modified NENL model of substorms.
- Published
- 2006
46. Survey of large-amplitude flapping motions in the midtail current sheet
- Author
-
D. A. Sormakov, Rumi Nakamura, Andrei Runov, Tokuo Mukai, V. A. Sergeev, S. Apatenkov, T. Nagai, Wolfgang Baumjohann, EGU, Publication, St Petersburg State University (SPbU), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), Department of Earth and Planetary Sciences [TITECH Tokyo], and Tokyo Institute of Technology [Tokyo] (TITECH)
- Subjects
Atmospheric Science ,010504 meteorology & atmospheric sciences ,[SDU.STU]Sciences of the Universe [physics]/Earth Sciences ,Perturbation (astronomy) ,Electrojet ,01 natural sciences ,Current sheet ,0103 physical sciences ,Substorm ,Earth and Planetary Sciences (miscellaneous) ,lcsh:Science ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences ,[SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere ,Physics ,[SDU.OCEAN] Sciences of the Universe [physics]/Ocean, Atmosphere ,lcsh:QC801-809 ,Plasma sheet ,Geology ,Astronomy and Astrophysics ,Geophysics ,Geodesy ,lcsh:QC1-999 ,lcsh:Geophysics. Cosmic physics ,Amplitude ,Flow velocity ,Space and Planetary Science ,[SDU.STU] Sciences of the Universe [physics]/Earth Sciences ,Flapping ,lcsh:Q ,lcsh:Physics - Abstract
We surveyed fast current sheet crossings (flapping motions) over the distance range 10–30 RE in the magnetotail covered by the Geotail spacecraft. Since the local tilts of these dynamic sheets are large and variable in these events, we compare three different methods of evaluating current sheet normals using 4-s/c Cluster data and define the success criteria for the single-spacecraft-based method (MVA) to obtain the reliable results. Then, after identifying more than ~1100 fast CS crossings over a 3-year period of Geotail observations in 1997–1999, we address their parameters, spatial distribution and activity dependence. We confirm that over the entire distance covered and LT bins, fast crossings have considerable tilts in the YZ plane (from estimated MVA normals) which show a preferential appearance of one (YZ kink-like) mode that is responsible for these severe current sheet perturbations. Their occurrence is highly inhomogeneous; it sharply increases with radial distance and has a peak in the tail center (with some duskward shift), resembling the occurrence of the BBFs, although there is no one-to-one local correspondence between these two phenomena. The crossing durations typically spread around 1 min and decrease significantly where the high-speed flows are registered. Based on an AE index superposed epoch study, the flapping motions prefer to appear during the substorm expansion phase, although a considerable number of events without any electrojet and auroral activity were also observed. We also present statistical distributions of other parameters and briefly discuss what could be possible mechanisms to generate the flapping motions.
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- 2006
47. A statistical survey of the magnetotail current sheet
- Author
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Rumi Nakamura, Junru Shi, Hans Eichelberger, Zoltán Vörös, Martin Volwerk, Y. Asano, V. A. Sergeev, Andrei Runov, Wolfgang Baumjohann, André Balogh, and Tinglong Zhang
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Physics ,Atmospheric Science ,Spacecraft ,business.industry ,Magnetometer ,Superposed epoch analysis ,Aerospace Engineering ,Astronomy and Astrophysics ,Geodesy ,law.invention ,Current sheet ,Geophysics ,Space and Planetary Science ,law ,Physics::Space Physics ,General Earth and Planetary Sciences ,Heliospheric current sheet ,Atomic physics ,Current (fluid) ,business ,Current density ,Statistical survey - Abstract
Using Cluster magnetometer data during summer 2001 and 2002, when the spacecraft traversed the magnetotail, we have performed a survey of current sheet and its current. We applied a superposed epoch analysis to simple, monotonous current sheet crossings and obtained a statistical profile of the current sheet. We find that the averaged structure of the current sheet fits well with the Harris current sheet description. By using the four spacecraft measurements, the current is calculated and a statistical current density profile of the current sheet is produced.
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- 2006
48. A reconstruction method for the reconnection rate applied to Cluster magnetotail measurements
- Author
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V. A. Sergeev, V.V. Ivanova, Rumi Nakamura, Martin Heyn, Vladimir Semenov, Helfried K. Biernat, Thomas Penz, I. B. Ivanov, and I. V. Kubyshkin
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Physics ,Atmospheric Science ,Plasma sheet ,Aerospace Engineering ,Flux ,Astronomy and Astrophysics ,Magnetic reconnection ,Plasma ,Inverse problem ,Regularization (mathematics) ,Computational physics ,Magnetic field ,Geophysics ,Classical mechanics ,Physics::Plasma Physics ,Space and Planetary Science ,Position (vector) ,Physics::Space Physics ,General Earth and Planetary Sciences - Abstract
We apply a theoretical model to describe the behavior of nightside flux transfer events (NFTEs) measured by Cluster satellites in the Earth magnetotail. Based on the Cagniard–deHoop method we calculate the magnetic field and plasma flow time series observed by a satellite. Our aim is to solve an inverse problem to obtain the reconnection rate from the measured plasma data. The ill-posed inverse problem is treated with the method of regularization, since the solution of the Cagniard–deHoop method is given in the form of a convolution integral, which is well known in the theory of inverse problems. This method is applied to Cluster measurements from September 8th, 2002, where a series of Earthward propagating 1-min scale magnetic field and plasma flow variations were observed outside of the plasma sheet, which are consistent with the theoretical picture of NFTEs. Estimations of the satellite position with respect to the reconnection site and of the Alfven velocity are made because they are necessary parameters for the model. The reconnection rate is found to be in the range of 1–2 mV/m and the reconnection site at about 29 Re tailwards.
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- 2006
49. Statistical study of the proton isotropy boundary
- Author
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E. A. Lvova, V. A. Sergeev, G. R. Bagautdinova, Institute of Physics, Czech Academy of Sciences [Prague] (CAS), and EGU, Publication
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Atmospheric Science ,010504 meteorology & atmospheric sciences ,Magnetosphere ,Boundary (topology) ,[SDU.STU]Sciences of the Universe [physics]/Earth Sciences ,01 natural sciences ,Relativistic particle ,0103 physical sciences ,Earth and Planetary Sciences (miscellaneous) ,Astrophysics::Solar and Stellar Astrophysics ,lcsh:Science ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences ,Physics ,[SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere ,[SDU.OCEAN] Sciences of the Universe [physics]/Ocean, Atmosphere ,Isotropy ,lcsh:QC801-809 ,Geology ,Astronomy and Astrophysics ,Geophysics ,lcsh:QC1-999 ,Computational physics ,Solar wind ,lcsh:Geophysics. Cosmic physics ,Amplitude ,13. Climate action ,Space and Planetary Science ,Physics::Space Physics ,[SDU.STU] Sciences of the Universe [physics]/Earth Sciences ,Polar ,Dynamic pressure ,lcsh:Q ,lcsh:Physics - Abstract
Based on a large data set of polar NOAA-type satellite observations we studied the latitude-MLT shape of the 80keV proton isotropy boundary (IB) as a function of the solar wind parameters and magnetic activity. Using "snapshots" of isotropy boundaries near-simultaneously crossed at four points we found that its equatorward expansion, as well as its dawn-dusk shift, depends mostly on the AE-index and on the corrected Dst*, whereas the amplitude of the IB daily variation is mostly controlled by the solar wind dynamic pressure. Applying a nonlinear, multi-parametric, least-square regression procedure, the empirical relationship describing the IB latitude as a function of MLT and AE, Pd, Dst* parameters was obtained. Comparing it with the predictions from the Tsyganenko-2001 model we found a good agreement during the quiet time but some important differences during the disturbed periods. Interpretation of these results in terms of the properties of the magnetospheric configuration is briefly discussed.
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- 2005
50. Electric current and magnetic field geometry in flapping magnetotail current sheets
- Author
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A. Runov, V. A. Sergeev, W. Baumjohann, R. Nakamura, S. Apatenkov, Y. Asano, M. Volwerk, Z. Vörös, T. L. Zhang, A. Petrukovich, A. Balogh, J.-A. Sauvaud, B. Klecker, H. Rème, Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), St Petersburg State University (SPbU), Max-Planck-Institut für Extraterrestrische Physik (MPE), Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Imperial College London, Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées
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Atmospheric Science ,010504 meteorology & atmospheric sciences ,[SDU.STU]Sciences of the Universe [physics]/Earth Sciences ,Curvature ,01 natural sciences ,Current sheet ,0103 physical sciences ,Earth and Planetary Sciences (miscellaneous) ,lcsh:Science ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences ,[SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere ,Physics ,lcsh:QC801-809 ,Plasma sheet ,Geology ,Astronomy and Astrophysics ,Geophysics ,lcsh:QC1-999 ,Computational physics ,Magnetic field ,lcsh:Geophysics. Cosmic physics ,Space and Planetary Science ,Physics::Space Physics ,Vector field ,lcsh:Q ,Heliospheric current sheet ,Electric current ,Current density ,lcsh:Physics - Abstract
Using four-point magnetic field measurements by the Cluster spacecraft, we statistically analyze the magnetic field and electric current configurations during rapid crossings of the current sheet observed in July-October 2001 at geocentric distances of 19 RE. The database includes 78 crossings, specially selected to apply multi-point data analysis techniques to calculate vector derivatives. Observed bipolar variations of jz, often with | jz |>jy, indicate that the electric currents follow kinks of the current sheet. The current density varies between 5-25nA/m2. The half-thickness of the current sheet during flapping varies over a wide range, from 1 to 20 ion thermal gyroradii (Lcp), calculated from average temperature and lobe magnetic field for each crossing). We found no relationship between the tilt angle of the current sheet normal and the half-thickness. In 68 cases the magnetic field curvature vector has a positive (earthward) X-component. Ten cases with a negative (tailward) curvature, associated with reconnection, were detected within 0
- Published
- 2005
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