94 results on '"Eino Valtonen"'
Search Results
2. Relationships between energetic storm particle events and interplanetary shocks driven by full and partial halo coronal mass ejections
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Dheyaa Ameri, Eino Valtonen, Amjad Al-Sawad, and Rami Vainio
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Atmospheric Science ,Geophysics ,Space and Planetary Science ,Aerospace Engineering ,General Earth and Planetary Sciences ,Astronomy and Astrophysics - Published
- 2023
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3. Erratum: Properties of a New Group of Cosmic Nuclei: Results from the Alpha Magnetic Spectrometer on Sodium, Aluminum, and Nitrogen [Phys. Rev. Lett. 127 , 021101 (2021)]
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Massimo Gervasi, I. Lazzizzera, C. Mañá, Veronica Bindi, Corrado Gargiulo, M. Molero, M. Capell, J. Marquardt, Alexandre Lebedev, E. Fiandrini, T. Kirn, Yi-Cong Yu, Y. Yang, F. Machate, Fajun Zhang, S. C. Lee, J. J. Torsti, S. Pensotti, Antonino Zichichi, H. Y. Chou, H. T. Lee, M. Pohl, Ilya Usoskin, Z. Cui, C. H. Chung, V. Formato, Zheng Wang, M. Bourquin, L. Wang, G. N. Kim, Zhihua Zhang, Rami Vainio, Paolo Zuccon, M. Graziani, H. L. Zhuang, C. Consolandi, Valerio Vagelli, M Valencia-Otero, W. J. Burger, Pier-Giorgio Rancoita, P. Mott, M. Incagli, F. Cervelli, Arturo Alejandro Menchaca-Rocha, J. W. Song, M. Duranti, R. Q. Xiong, F. Barao, K. C. Han, M. Behlmann, E. Valente, H. D. Phan, F. Zhao, K. Dadzie, R. Sonnabend, N. Nikonov, J Liang, S. Li, Chuanguo Zhang, B. Khiali, Mayda Velasco, J. H. Zhang, S. Chouridou, Q. L. Wang, J. Casaus, C. Delgado, Lin Cheng, Elisa Laudi, Zhen Sun, L Mussolin, S. Di Falco, M. Paniccia, E. F. Bueno, Jun Liu, Jianfeng Feng, Maxim Konyushikhin, Valery Zhukov, D. M. Gómez-Coral, Timothy H. Hsieh, N. Attig, L Strigari, G. La Vacca, F. Giovacchini, V. Choutko, G. Ambrosi, M. Li, S. Wang, David Maurin, Mario Zannoni, C. Gámez, D. Krasnopevtsev, A. Kuhlman, J Tian, Thomas Lippert, Z. H. He, F. Nozzoli, J. D. Burger, T. Siedenburg, Samuel C.C. Ting, B Beranek, Zhixiang Tang, N. Masi, Bernd Heber, L. Barrin, Z. Y. Qu, P. H. Fisher, R. J. García-López, W. Xu, V. Di Felice, S. M. Ting, P. von Doetinchem, Xi Luo, X. D. Cai, J Negrete, Claudio Corti, A. Schulz von Dratzig, Z. Q. Yu, G. Castellini, K. Bollweg, G. Laurenti, C X Wang, Z Liu, Z. L. Weng, D. Rapin, Laurent Derome, V. Plyaskin, F. Dong, R. K. Hashmani, Xubo Qin, K. Luebelsmeyer, Qie Sun, C. Solano, S. Q. Lu, F. Donnini, C. Freeman, Stefan Schael, Yu Wang, F. Palmonari, A. Egorov, M. Pauluzzi, Z Shakfa, Carlos Díaz, Mauro Tacconi, B. S. Shan, Bruna Bertucci, H. S. Chen, M. B. Demirköz, G R Chen, Andrei Kounine, Q. Yan, S. Başeğmez-du Pree, Naihua Wang, A. Pashnin, Jun Hu, J Wei, M. Palermo, T. Urban, O. Kounina, H. Wu, Luísa Arruda, M. Aguilar, G. Coignet, Roald Z. Sagdeev, Julio C. Marín, Y. Chen, Yi Jia, Eun-Suk Seo, X. Q. Wang, Andrea Contin, Ying Lu, H. Jinchi, S. Della Torre, A.I. Oliva, Y. H. Chang, S. Rosier-Lees, T Su, V. Koutsenko, Eino Valtonen, A. Kulemzin, G. Schwering, V. V. Mikhailov, Stepan Poluianov, L. Ali Cavasonza, S. Burmeister, D. Rozza, F. Dimiccoli, X J Song, J. Z. Luo, A. Bartoloni, Z. H. Li, Qiang Li, Liqiu Wang, Lucio Quadrani, J. Berdugo, D. Grandi, J H Li, E Robyn, Fan Zhang, M. Vazquez Acosta, I. I. Yashin, A. Eline, M. Orcinha, Manuela Vecchi, C Zheng, G. Martinez, C. Clark, W. Y. Jang, Guo-Ming Chen, Chia-Hui Lin, J. Gong, C. Goy, H. Yi, Roberto Battiston, B. Borgia, Q. Meng, Henning Gast, Tim Martin, Sadakazu Haino, C. Tüysüz, A. Rozhkov, Varlen Grabski, A. Reina Conde, X. W. Tang, Jinglai Li, J. P. Vialle, M. J. Boschini, Z. M. Zheng, C. Light, Nicola Tomassetti, Tatiana Medvedeva, and Behcet Alpat
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Physics ,COSMIC cancer database ,Cosmic ray composition & spectra ,Sodium ,Analytical chemistry ,General Physics and Astronomy ,chemistry.chemical_element ,Cosmic ray sources ,Nitrogen ,Cosmic ray acceleration, Cosmic ray composition & spectra, Cosmic ray propagation, Cosmic ray sources, Gravitation, Cosmology & Astrophysics [Physics Subject Headings (PhySH)] ,Cosmology & Astrophysics ,chemistry ,Group (periodic table) ,Aluminium ,Cosmic ray acceleration [Physics Subject Headings (PhySH)] ,Cosmic ray propagation ,Alpha Magnetic Spectrometer ,ddc:530 ,Gravitation - Published
- 2021
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4. Potential role of energetic particle observations in geomagnetic storm forecasting
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Dheyaa Ameri and Eino Valtonen
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Physics ,Geomagnetic storm ,Atmospheric Science ,010504 meteorology & atmospheric sciences ,Solar energetic particles ,Aerospace Engineering ,Solar cycle 23 ,Astronomy and Astrophysics ,Storm ,Solar cycle 24 ,Atmospheric sciences ,01 natural sciences ,Standard deviation ,Geophysics ,Space and Planetary Science ,0103 physical sciences ,Coronal mass ejection ,General Earth and Planetary Sciences ,Interplanetary spaceflight ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences - Abstract
We have searched for solar proton events consisting of both solar energetic particles (SEPs) accelerated near the Sun and energetic storm particles (ESPs) accelerated by interplanetary shocks driven by coronal mass ejections (CMEs) and observed near the time when the shock passes the observer. The purpose of this study is to investigate the possibilities and advantages of using energetic particle observations for mid-term (warning time several hours) forecasting of geomagnetic storms or as a support for longer-term forecasting methods based on solar observations. The study period extends from May 1996 to December 2017 covering the entire solar cycle 23 and the major part of solar cycle 24. Using two particle energies, 2 and 20 MeV, we found 95 SEP–ESP events of which 65 were associated with geomagnetic storms with Dst ⩽ −50 nT caused by CMEs. We performed correlation analysis between log10|Dst (nT)| and various parameters characterising the particle events or the associated CMEs. We found the best correlations for the single independent variables Δ t ESP - SEP ( r = - 0.47 ± 0.08 ), which is the difference between the ESP peak time and SEP onset time, the CME direction parameter DP ( r = 0.47 ± 0.10 ), and the logarithm of the maximum ESP energy log10[ E ESP max (MeV)] ( r = 0.44 ± 0.11 ). Using a linear combination of these three variables improves the correlation ( r = 0.68 ± 0.07 ). We suggest that an empirical equation based on these three parameters and requiring only coronagraph observations of CMEs and energetic particle measurements in interplanetary space can be used for mid-term forecasting of geomagnetic storm strengths. We found that 74% of the strongest storms (Dst ⩽ - 200 nT) during the study period were associated with energetic particle events. The average warning time and its standard deviation for all geomagnetic storms associated with SEP–ESP events was ( 15 ± 10 ) hours.
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- 2019
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5. Properties of a New Group of Cosmic Nuclei: Results from the Alpha Magnetic Spectrometer on Sodium, Aluminum, and Nitrogen
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Roberto Battiston, N. Nikonov, T. Martin, J. W. Song, M. Vecchi, M. Duranti, G. N. Kim, Zhihua Zhang, J. Casaus, H. L. Zhuang, B. Borgia, M. Pauluzzi, Corrado Gargiulo, H. Jinchi, D. Grandi, M. Paniccia, S. C. Lee, M. Bourquin, J Tian, Bernd Heber, G. Schwering, E Robyn, B. Bertucci, L Mussolin, M. Vazquez Acosta, C X Wang, Yichao Yu, D M Gómez-Coral, Ignazio Lazzizzera, C. Gámez, R. Q. Xiong, G. Martinez, C. Freeman, L. Ali Cavasonza, Fan Zhang, O. Kounina, H. Wu, Samuel C.C. Ting, B Beranek, K. Bollweg, Qie Sun, Mayda Velasco, S. Başeğmez-du Pree, Corinne Goy, Yung Huang Chang, K. Luebelsmeyer, G. Laurenti, J. Z. Luo, Lucio Quadrani, Liqiu Wang, C. Solano, E F Bueno, I. I. Yashin, Jun Liu, H. S. Chen, Z. H. He, Roald Z. Sagdeev, S. Della Torre, P. von Doetinchem, Andrea Contin, X. D. Cai, F. Nozzoli, G R Chen, A. Kulemzin, M. Palermo, G. Coignet, Z Liu, J Wei, Z. L. Weng, S. Rosier-Lees, R. J. García-López, Valery Zhukov, D. Rapin, V. Plyaskin, Matteo Boschini, M. Pohl, C. Consolandi, V. Formato, Mauro Tacconi, V. Di Felice, A. Egorov, J. D. Burger, T. Siedenburg, B. S. Shan, M. Konyushikhin, M. B. Demirköz, Youhua Yang, Z Shakfa, Rami Vainio, V Vagelli, F. Donnini, H. D. Phan, F. Zhao, C Zheng, Massimo Gervasi, H. T. Lee, Carlos Díaz, J. Berdugo, J Negrete, Claudio Corti, F. Dimiccoli, Yi Jia, Elisa Laudi, Lin Cheng, Mario Zannoni, Stefan Schael, J Liang, Z. Y. Qu, L. Wang, Andrei Kounine, Q. Yan, M. Graziani, B. Khiali, Timothy H. Hsieh, T. Urban, M. Li, J H Li, J. H. Zhang, D. Rozza, C. Light, N. Attig, Pier-Giorgio Rancoita, A. Pashnin, M. Capell, V. Choutko, C. Mañá, G. Ambrosi, C. H. Chung, J. Marquardt, Xi Luo, Naihua Wang, T Medvedeva, J. J. Torsti, S. Pensotti, Veronica Bindi, G. Castellini, M Valencia-Otero, S. Li, W. J. Burger, K. C. Han, M. Molero, F. Cervelli, E. Fiandrini, X. Qin, S. Di Falco, Q. L. Wang, W Xu, S Wang, C. Delgado, T. Kirn, Nicola Tomassetti, F. Giovacchini, D. Krasnopevtsev, P. Mott, M. Behlmann, Luísa Arruda, Behcet Alpat, Julio C. Marín, A. Lebedev, Zhixiang Tang, A. Menchaca-Rocha, Ilya Usoskin, S. Chouridou, J. Q. Li, A. Kuhlman, A.I. Oliva, M. Orcinha, F. Barao, L Strigari, X. W. Tang, Thomas Lippert, M. Incagli, R. K. Hashmani, P. H. Fisher, S. M. Ting, Xiaoqun Wang, K. Dadzie, F. Palmonari, J. P. Vialle, Zhenzi Wang, Z. M. Zheng, F. Machate, H. Y. Chou, Z. Cui, Q. Meng, Yu Wang, Sadakazu Haino, C. Tüysüz, M. Aguilar, R. Sonnabend, W. Y. Jang, Guo-Ming Chen, Chia-Hui Lin, J. Gong, S. Q. Lu, H. Yi, Henning Gast, S. Burmeister, X J Song, A. Bartoloni, A. Rozhkov, Varlen Grabski, Jun Hu, A. Reina Conde, Eun-Suk Seo, Ying Lu, P. Zuccon, V. Koutsenko, Eino Valtonen, Z. H. Li, Qiang Li, C. Clark, A. Eline, E. Valente, Chuanguo Zhang, N. Masi, L. Barrin, A. Schulz von Dratzig, Z. Q. Yu, F. Dong, Y. Chen, A. Zichichi, T Su, V. V. Mikhailov, Stepan Poluianov, Fajun Zhang, Jonathan L. Feng, Zhen Sun, G. La Vacca, David Maurin, Laurent Derome, Bourquin, Maurice, Chen, Yao, Liu, Zhen, Paniccia, Mercedes, Pohl, Martin, Rapin, Divic Jean, Robyn, Erwan, Wei, Jiahui, 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), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), AMS, Aguilar, M, Cavasonza, L, Alpat, B, Ambrosi, G, Arruda, L, Attig, N, Barao, F, Barrin, L, Bartoloni, A, Başeğmez-du Pree, S, Battiston, R, Behlmann, M, Beranek, B, Berdugo, J, Bertucci, B, Bindi, V, Bollweg, K, Borgia, B, Boschini, M, Bourquin, M, Bueno, E, Burger, J, Burger, W, Burmeister, S, Cai, X, Capell, M, Casaus, J, Castellini, G, Cervelli, F, Chang, Y, Chen, G, Chen, H, Chen, Y, Cheng, L, Chou, H, Chouridou, S, Choutko, V, Chung, C, Clark, C, Coignet, G, Consolandi, C, Contin, A, Corti, C, Cui, Z, Dadzie, K, Delgado, C, Della Torre, S, Demirköz, M, Derome, L, Di Falco, S, Di Felice, V, Díaz, C, Dimiccoli, F, von Doetinchem, P, Dong, F, Donnini, F, Duranti, M, Egorov, A, Eline, A, Feng, J, Fiandrini, E, Fisher, P, Formato, V, Freeman, C, Gámez, C, García-López, R, Gargiulo, C, Gast, H, Gervasi, M, Giovacchini, F, Gómez-Coral, D, Gong, J, Goy, C, Grabski, V, Grandi, D, Graziani, M, Haino, S, Han, K, Hashmani, R, He, Z, Heber, B, Hsieh, T, Hu, J, Incagli, M, Jang, W, Jia, Y, Jinchi, H, Khiali, B, Kim, G, Kirn, T, Konyushikhin, M, Kounina, O, Kounine, A, Koutsenko, V, Krasnopevtsev, D, Kuhlman, A, Kulemzin, A, La Vacca, G, Laudi, E, Laurenti, G, Lazzizzera, I, Lebedev, A, Lee, H, Lee, S, Li, J, Li, M, Li, Q, Li, S, Li, Z, Liang, J, Light, C, Lin, C, Lippert, T, Liu, J, Liu, Z, Lu, S, Lu, Y, Luebelsmeyer, K, Luo, J, Luo, X, Machate, F, Mañá, C, Marín, J, Marquardt, J, Martin, T, Martínez, G, Masi, N, Maurin, D, Medvedeva, T, Menchaca-Rocha, A, Meng, Q, Mikhailov, V, Molero, M, Mott, P, Mussolin, L, Negrete, J, Nikonov, N, Nozzoli, F, Oliva, A, Orcinha, M, Palermo, M, Palmonari, F, Paniccia, M, Pashnin, A, Pauluzzi, M, Pensotti, S, Phan, H, Plyaskin, V, Pohl, M, Poluianov, S, Qin, X, Qu, Z, Quadrani, L, Rancoita, P, Rapin, D, Conde, A, Robyn, E, Rosier-Lees, S, Rozhkov, A, Rozza, D, Sagdeev, R, Schael, S, von Dratzig, A, Schwering, G, Seo, E, Shakfa, Z, Shan, B, Siedenburg, T, Solano, C, Song, J, Song, X, Sonnabend, R, Strigari, L, Su, T, Sun, Q, Sun, Z, Tacconi, M, Tang, X, Tang, Z, Tian, J, Ting, S, Tomassetti, N, Torsti, J, Tüysüz, C, Urban, T, Usoskin, I, Vagelli, V, Vainio, R, Valencia-Otero, M, Valente, E, Valtonen, E, Vázquez Acosta, M, Vecchi, M, Velasco, M, Vialle, J, Wang, C, Wang, L, Wang, N, Wang, Q, Wang, S, Wang, X, Wang, Y, Wang, Z, Wei, J, Weng, Z, Wu, H, Xiong, R, Xu, W, Yan, Q, Yang, Y, Yashin, I, Yi, H, Yu, Y, Yu, Z, Zannoni, M, Zhang, C, Zhang, F, Zhang, J, Zhang, Z, Zhao, F, Zheng, C, Zheng, Z, Zhuang, H, Zhukov, V, Zichichi, A, Zuccon, P, Aguilar M., Cavasonza L.A., Alpat B., Ambrosi G., Arruda L., Attig N., Barao F., Barrin L., Bartoloni A., Basegmez-Du Pree S., Battiston R., Behlmann M., Beranek B., Berdugo J., Bertucci B., Bindi V., Bollweg K., Borgia B., Boschini M.J., Bourquin M., Bueno E.F., Burger J., Burger W.J., Burmeister S., Cai X.D., Capell M., Casaus J., Castellini G., Cervelli F., Chang Y.H., Chen G.M., Chen G.R., Chen H.S., Chen Y., Cheng L., Chou H.Y., Chouridou S., Choutko V., Chung C.H., Clark C., Coignet G., Consolandi C., Contin A., Corti C., Cui Z., Dadzie K., Delgado C., Della Torre S., Demirkoz M.B., Derome L., Di Falco S., Di Felice V., Diaz C., Dimiccoli F., Von Doetinchem P., Dong F., Donnini F., Duranti M., Egorov A., Eline A., Feng J., Fiandrini E., Fisher P., Formato V., Freeman C., Gamez C., Garcia-Lopez R.J., Gargiulo C., Gast H., Gervasi M., Giovacchini F., Gomez-Coral D.M., Gong J., Goy C., Grabski V., Grandi D., Graziani M., Haino S., Han K.C., Hashmani R.K., He Z.H., Heber B., Hsieh T.H., Hu J.Y., Incagli M., Jang W.Y., Jia Y., Jinchi H., Khiali B., Kim G.N., Kirn T., Konyushikhin M., Kounina O., Kounine A., Koutsenko V., Krasnopevtsev D., Kuhlman A., Kulemzin A., La Vacca G., Laudi E., Laurenti G., Lazzizzera I., Lebedev A., Lee H.T., Lee S.C., Li J.Q., Li M., Li Q., Li S., Li J.H., Li Z.H., Liang J., Light C., Lin C.H., Lippert T., Liu J.H., Liu Z., Lu S.Q., Lu Y.S., Luebelsmeyer K., Luo J.Z., Luo X., Machate F., Mana C., Marin J., Marquardt J., Martin T., Martinez G., Masi N., Maurin D., Medvedeva T., Menchaca-Rocha A., Meng Q., Mikhailov V.V., Molero M., Mott P., Mussolin L., Negrete J., Nikonov N., Nozzoli F., Oliva A., Orcinha M., Palermo M., Palmonari F., Paniccia M., Pashnin A., Pauluzzi M., Pensotti S., Phan H.D., Plyaskin V., Pohl M., Poluianov S., Qin X., Qu Z.Y., Quadrani L., Rancoita P.G., Rapin D., Conde A.R., Robyn E., Rosier-Lees S., Rozhkov A., Rozza D., Sagdeev R., Schael S., Von Dratzig A.S., Schwering G., Seo E.S., Shakfa Z., Shan B.S., Siedenburg T., Solano C., Song J.W., Song X.J., Sonnabend R., Strigari L., Su T., Sun Q., Sun Z.T., Tacconi M., Tang X.W., Tang Z.C., Tian J., Ting S.C.C., Ting S.M., Tomassetti N., Torsti J., Tuysuz C., Urban T., Usoskin I., Vagelli V., Vainio R., Valencia-Otero M., Valente E., Valtonen E., Vazquez Acosta M., Vecchi M., Velasco M., Vialle J.P., Wang C.X., Wang L., Wang L.Q., Wang N.H., Wang Q.L., Wang S., Wang X., Wang Y., Wang Z.M., Wei J., Weng Z.L., Wu H., Xiong R.Q., Xu W., Yan Q., Yang Y., Yashin I.I., Yi H., Yu Y.M., Yu Z.Q., Zannoni M., Zhang C., Zhang F., Zhang F.Z., Zhang J.H., Zhang Z., Zhao F., Zheng C., Zheng Z.M., Zhuang H.L., Zhukov V., Zichichi A., Zuccon P., and Astronomy
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Cosmic ray composition & spectra ,Analytical chemistry ,General Physics and Astronomy ,Cosmic Ray nuclei ,Galactic cosmic rays ,International Space Station ,01 natural sciences ,Cosmology & Astrophysics ,Alpha Magnetic Spectrometer ,Cosmic-rays ,AMS ,010303 astronomy & astrophysics ,Range (particle radiation) ,COSMIC cancer database ,Nitrogen ,Aluminum nuclei ,FIS/01 - FISICA SPERIMENTALE ,Cosmic ray propagation ,Gravitation ,Primary cosmic rays ,Materials science ,Silicon ,Cosmic-ray source abundance ,Astrophysics::High Energy Astrophysical Phenomena ,Sodium ,chemistry.chemical_element ,Cosmic ray ,ddc:500.2 ,Astrophysics::Cosmology and Extragalactic Astrophysics ,[PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex] ,Cosmic ray acceleration ,FIS/05 - ASTRONOMIA E ASTROFISICA ,Flux (metallurgy) ,cosmic rays ,Cosmic Nuclei ,AMS-02 ,0103 physical sciences ,ddc:530 ,Nuclear Physics - Experiment ,010306 general physics ,Cosmic ray acceleration, Cosmic ray composition & spectra, Cosmic ray propagation, Cosmic ray sources, Gravitation, Cosmology & Astrophysics ,Cosmic ray sources ,Sodium nuclei ,magnetic spectrometer ,Secondary cosmic rays ,chemistry ,Astroparticle physics ,Cosmic-ray nuclei ,Aluminum - Abstract
Physical review letters : PRL 127(15), 021101 (2021). doi:10.1103/PhysRevLett.127.021101, Published by American Physical Society, College Park, Md.
- Published
- 2021
- Full Text
- View/download PDF
6. The Alpha Magnetic Spectrometer (AMS) on the international space station : Part II : Results from the first seven years
- Author
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Roberto Battiston, X. M. Qi, R. Sonnabend, Massimo Gervasi, B. Borgia, M. Pohl, Rami Vainio, W. Hungerford, M. Vecchi, H. D. Phan, F. Zhao, M. Capell, J. Marquardt, Ignazio Lazzizzera, F. Barao, G. Schwering, C. Consolandi, Pier-Giorgio Rancoita, M. Pauluzzi, M. Graziani, Liqiu Wang, Y. J. Yu, S. Başeğmez-du Pree, V. Formato, Julio C. Marín, Xiaoqun Wang, Y. Yang, W Xu, F. Machate, M. Aguilar, H. Y. Chou, Z. Cui, K. C. Han, A. Pashnin, Thomas Lippert, K. H. Guo, A. Lebedev, S. Li, Q. L. Wang, Fan Zhang, Lin Cheng, S. Di Falco, Z Liu, G. Ambrosi, A. Kuhlman, S Wang, C. Delgado, P. H. Fisher, Roald Z. Sagdeev, S. M. Ting, Z. L. Weng, D. Rapin, V. Plyaskin, Corrado Gargiulo, F. Giovacchini, X. W. Tang, C. Freeman, S. Della Torre, S. Porter, S. S. Lyu, Timothy H. Hsieh, S. Rosier-Lees, P. Mott, Ilya Usoskin, Mauro Tacconi, F. Palmonari, B. S. Shan, Zhixiang Tang, M. B. Demirköz, M. Li, Zhiqi Huang, E. Valente, J. Q. Li, M. Konyushikhin, Chuanguo Zhang, Zhen Sun, G. N. Kim, Zhihua Zhang, Yi Jia, N. Attig, O. Kounina, H. Wu, J. P. Vialle, R. K. Hashmani, Naihua Wang, H. L. Zhuang, Valery Zhukov, S. C. Lee, C. Clark, Z. Y. Qu, Andrea Contin, G. Coignet, S. Chouridou, C. Leluc, R. J. García-López, J. D. Burger, S. M. Schmidt, L Mussolin, T. Siedenburg, G. Martinez, J. J. Torsti, S. Pensotti, Antonino Zichichi, M. Orcinha, F. Dimiccoli, Yaomin Dai, G. La Vacca, M. Incagli, Corinne Goy, Z. M. Zheng, K. Bollweg, G. Castellini, J Wei, L. Ali Cavasonza, S. Q. Lu, J. Z. Luo, Claudio Corti, M. Vazquez Acosta, K. Dadzie, Yung Huang Chang, A.I. Oliva, Qie Sun, C. Solano, V. Choutko, Z. H. He, F. Nozzoli, K. Luebelsmeyer, A. Kulemzin, A. Eline, X. Qin, David Maurin, B. Beischer, C. Mañá, Veronica Bindi, V. Di Felice, J. Y. Shi, G. Laurenti, M. Molero, Jun Hu, Arturo Alejandro Menchaca-Rocha, J. Berdugo, E. Fiandrini, T. Kirn, C. Light, H. S. Chen, L. Quadrani, Luísa Arruda, S. Burmeister, M. Bourquin, B. Khiali, Eun-Suk Seo, M. Palermo, Ying Lu, A. Bartoloni, J. Bates, J. H. Zhang, Mario Zannoni, K. Kanishev, Nicola Tomassetti, P. Zuccon, V. Koutsenko, Eino Valtonen, T. Urban, R. Q. Xiong, Z. H. Li, Qiang Li, Mayda Velasco, H. Jinchi, D M Gómez-Coral, D. Grandi, S. Schael, B. Bertucci, C. H. Chung, C. Gámez, D. C. Mo, N. Masi, L. Barrin, M. Behlmann, P. von Doetinchem, X. D. Cai, Elisa Laudi, Laurent Derome, Q. Meng, F. Donnini, A. Schulz von Dratzig, Andrei Kounine, Q. Yan, Sadakazu Haino, C. Tüysüz, N. Zimmermann, Zhao Wang, Z. Q. Yu, F. Dong, Fajun Zhang, Jonathan L. Feng, V Vagelli, Y. Chen, N. Nikonov, T. Martin, J. W. Song, M. Duranti, J. Casaus, J. Q. Ni, E F Bueno, A. Egorov, M. Paniccia, J Tian, Carlos Díaz, Bernd Heber, W. De Boer, H. Yi, Yu. Galaktionov, H. T. Lee, D. Rozza, W. J. Burger, Samuel C.C. Ting, F. Cervelli, Matteo Boschini, Henning Gast, A. Rozhkov, T. X. Li, Varlen Grabski, A. Reina Conde, I. Gebauer, W. Y. Jang, Guo-Ming Chen, Chia-Hui Lin, J. Gong, 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), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), AMS, Aguilar M., Ali Cavasonza L., Ambrosi G., Arruda L., Attig N., Barao F., Barrin L., Bartoloni A., Basegmez-du Pree S., Bates J., Battiston R., Behlmann M., Beischer B., Berdugo J., Bertucci B., Bindi V., de Boer W., Bollweg K., Borgia B., Boschini M.J., Bourquin M., Bueno E.F., Burger J., Burger W.J., Burmeister S., Cai X.D., Capell M., Casaus J., Castellini G., Cervelli F., Chang Y.H., Chen G.M., Chen H.S., Chen Y., Cheng L., Chou H.Y., Chouridou S., Choutko V., Chung C.H., Clark C., Coignet G., Consolandi C., Contin A., Corti C., Cui Z., Dadzie K., Dai Y.M., Delgado C., Della Torre S., Demirkoz M.B., Derome L., Di Falco S., Di Felice V., Diaz C., Dimiccoli F., von Doetinchem P., Dong F., Donnini F., Duranti M., Egorov A., Eline A., Feng J., Fiandrini E., Fisher P., Formato V., Freeman C., Galaktionov Y., Gamez C., Garcia-Lopez R.J., Gargiulo C., Gast H., Gebauer I., Gervasi M., Giovacchini F., Gomez-Coral D.M., Gong J., Goy C., Grabski V., Grandi D., Graziani M., Guo K.H., Haino S., Han K.C., Hashmani R.K., He Z.H., Heber B., Hsieh T.H., Hu J.Y., Huang Z.C., Hungerford W., Incagli M., Jang W.Y., Jia Y., Jinchi H., Kanishev K., Khiali B., Kim G.N., Kirn T., Konyushikhin M., Kounina O., Kounine A., Koutsenko V., Kuhlman A., Kulemzin A., La Vacca G., Laudi E., Laurenti G., Lazzizzera I., Lebedev A., Lee H.T., Lee S.C., Leluc C., Li J.Q., Li M., Li Q., Li S., Li T.X., Li Z.H., Light C., Lin C.H., Lippert T., Liu Z., Lu S.Q., Lu Y.S., Luebelsmeyer K., Luo J.Z., Lyu S.S., Machate F., Mana C., Marin J., Marquardt J., Martin T., Martinez G., Masi N., Maurin D., Menchaca-Rocha A., Meng Q., Mo D.C., Molero M., Mott P., Mussolin L., Ni J.Q., Nikonov N., Nozzoli F., Oliva A., Orcinha M., Palermo M., Palmonari F., Paniccia M., Pashnin A., Pauluzzi M., Pensotti S., Phan H.D., Plyaskin V., Pohl M., Porter S., Qi X.M., Qin X., Qu Z.Y., Quadrani L., Rancoita P.G., Rapin D., Reina Conde A., Rosier-Lees S., Rozhkov A., Rozza D., Sagdeev R., Schael S., Schmidt S.M., Schulz von Dratzig A., Schwering G., Seo E.S., Shan B.S., Shi J.Y., Siedenburg T., Solano C., Song J.W., Sonnabend R., Sun Q., Sun Z.T., Tacconi M., Tang X.W., Tang Z.C., Tian J., Ting S.C.C., Ting S.M., Tomassetti N., Torsti J., Tuysuz C., Urban T., Usoskin I., Vagelli V., Vainio R., Valente E., Valtonen E., Vazquez Acosta M., Vecchi M., Velasco M., Vialle J.P., Wang L.Q., Wang N.H., Wang Q.L., Wang S., Wang X., Wang Z.X., Wei J., Weng Z.L., Wu H., Xiong R.Q., Xu W., Yan Q., Yang Y., Yi H., Yu Y.J., Yu Z.Q., Zannoni M., Zhang C., Zhang F., Zhang F.Z., Zhang J.H., Zhang Z., Zhao F., Zheng Z.M., Zhuang H.L., Zhukov V., Zichichi A., Zimmermann N., Zuccon P., Aguilar, M, Ali Cavasonza, L, Ambrosi, G, Arruda, L, Attig, N, Barao, F, Barrin, L, Bartoloni, A, Başeğmez-du Pree, S, Bates, J, Battiston, R, Behlmann, M, Beischer, B, Berdugo, J, Bertucci, B, Bindi, V, de Boer, W, Bollweg, K, Borgia, B, Boschini, M, Bourquin, M, Bueno, E, Burger, J, Burger, W, Burmeister, S, Cai, X, Capell, M, Casaus, J, Castellini, G, Cervelli, F, Chang, Y, Chen, G, Chen, H, Chen, Y, Cheng, L, Chou, H, Chouridou, S, Choutko, V, Chung, C, Clark, C, Coignet, G, Consolandi, C, Contin, A, Corti, C, Cui, Z, Dadzie, K, Dai, Y, Delgado, C, Della Torre, S, Demirköz, M, Derome, L, Di Falco, S, Di Felice, V, Díaz, C, Dimiccoli, F, von Doetinchem, P, Dong, F, Donnini, F, Duranti, M, Egorov, A, Eline, A, Feng, J, Fiandrini, E, Fisher, P, Formato, V, Freeman, C, Galaktionov, Y, Gámez, C, García-López, R, Gargiulo, C, Gast, H, Gebauer, I, Gervasi, M, Giovacchini, F, Gómez-Coral, D, Gong, J, Goy, C, Grabski, V, Grandi, D, Graziani, M, Guo, K, Haino, S, Han, K, Hashmani, R, He, Z, Heber, B, Hsieh, T, Hu, J, Huang, Z, Hungerford, W, Incagli, M, Jang, W, Jia, Y, Jinchi, H, Kanishev, K, Khiali, B, Kim, G, Kirn, T, Konyushikhin, M, Kounina, O, Kounine, A, Koutsenko, V, Kuhlman, A, Kulemzin, A, La Vacca, G, Laudi, E, Laurenti, G, Lazzizzera, I, Lebedev, A, Lee, H, Lee, S, Leluc, C, Li, J, Li, M, Li, Q, Li, S, Li, T, Li, Z, Light, C, Lin, C, Lippert, T, Liu, Z, Lu, S, Lu, Y, Luebelsmeyer, K, Luo, J, Lyu, S, Machate, F, Mañá, C, Marín, J, Marquardt, J, Martin, T, Martínez, G, Masi, N, Maurin, D, Menchaca-Rocha, A, Meng, Q, Mo, D, Molero, M, Mott, P, Mussolin, L, Ni, J, Nikonov, N, Nozzoli, F, Oliva, A, Orcinha, M, Palermo, M, Palmonari, F, Paniccia, M, Pashnin, A, Pauluzzi, M, Pensotti, S, Phan, H, Plyaskin, V, Pohl, M, Porter, S, Qi, X, Qin, X, Qu, Z, Quadrani, L, Rancoita, P, Rapin, D, Reina Conde, A, Rosier-Lees, S, Rozhkov, A, Rozza, D, Sagdeev, R, Schael, S, Schmidt, S, Schulz von Dratzig, A, Schwering, G, Seo, E, Shan, B, Shi, J, Siedenburg, T, Solano, C, Song, J, Sonnabend, R, Sun, Q, Sun, Z, Tacconi, M, Tang, X, Tang, Z, Tian, J, Ting, S, Tomassetti, N, Torsti, J, Tüysüz, C, Urban, T, Usoskin, I, Vagelli, V, Vainio, R, Valente, E, Valtonen, E, Vázquez Acosta, M, Vecchi, M, Velasco, M, Vialle, J, Wang, L, Wang, N, Wang, Q, Wang, S, Wang, X, Wang, Z, Wei, J, Weng, Z, Wu, H, Xiong, R, Xu, W, Yan, Q, Yang, Y, Yi, H, Yu, Y, Yu, Z, Zannoni, M, Zhang, C, Zhang, F, Zhang, J, Zhang, Z, Zhao, F, Zheng, Z, Zhuang, H, Zhukov, V, Zichichi, A, Zimmermann, N, Zuccon, P, Astronomy, Bourquin, Maurice, Chen, Yao, Leluc, Catherine, Liu, Zhen, Paniccia, Mercedes, Pohl, Martin, Rapin, Divic Jean, and Wei, Jiahui
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Space station ,detector [cosmic radiation] ,electron ,Cosmic ray composition & spectra ,General Physics and Astronomy ,Transition radiation detector ,Strangelets ,positron: flux ,01 natural sciences ,Space detectors ,cosmic radiation: detector ,Cosmic ray detectors ,Alpha Magnetic Spectrometer ,antimatter ,Cosmic ray source ,AMS ,Particle astrophysic ,Physics ,cosmic radiation: propagation ,anti-p ,FIS/01 - FISICA SPERIMENTALE ,Antimatter ,Cosmic ray propagation ,positron ,acceleration [cosmic radiation] ,Particle astrophysics ,Cosmic ray composition & spectra, Cosmic ray acceleration, Cosmic ray propagation, Cosmic ray sources, Particle astrophysics, Particle dark matter, Cosmic ray detectors, Alpha Magnetic Spectrometer, International space station ,Astrophysics and Astronomy ,spectra ,Astrophysics::High Energy Astrophysical Phenomena ,Dark matter ,satellite ,Space Shuttle ,Cosmic ray ,ddc:500.2 ,Cosmic ray acceleration ,dark matter ,Nuclear physics ,Time of flight ,Ring imaging cherenkov ,FIS/05 - ASTRONOMIA E ASTROFISICA ,Particle dark matter ,Electromagnetic calorimeter ,0103 physical sciences ,International Space Station ,Cosmic ray composition & ,ddc:530 ,cosmic radiation: acceleration ,010306 general physics ,Cosmic rays ,Astroparticle physics ,010308 nuclear & particles physics ,International space station ,nucleus ,electron: flux ,Cosmic ray sources ,magnetic spectrometer ,Cosmic ray physics ,Automatic Keywords ,Antiproton ,Silicon tracker ,propagation [cosmic radiation] ,Cosmic ray detector ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] - Abstract
Physics reports 894, 1-116 (2021). doi:10.1016/j.physrep.2020.09.003 special issue: "The Alpha Magnetic Spectrometer (AMS) on the International Space Station: Part II : Results from the First Seven Years", Published by Elsevier Science, North-Holland, Amsterdam [u.a.]
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- 2021
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7. Properties of Iron Primary Cosmic Rays: Results from the Alpha Magnetic Spectrometer
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M. Li, N. Attig, Jun Hu, J Wei, Naihua Wang, J. J. Torsti, S. Pensotti, S. M. Ting, Eun-Suk Seo, G. Castellini, Ying Lu, E Robyn, X. Qin, P. Zuccon, V. Koutsenko, Eino Valtonen, Fan Zhang, A. Menchaca-Rocha, A.I. Oliva, I. I. Yashin, Z. H. Li, A. Egorov, G. N. Kim, Zhihua Zhang, S. S. Lyu, E. Fiandrini, M. Konyushikhin, Z. Y. Qu, H. S. Chen, Qiang Li, Z Shakfa, M. Orcinha, C. Clark, G. Schwering, Rami Vainio, W. Y. Jang, Guo-Ming Chen, Chia-Hui Lin, Julio C. Marín, O. Kounina, Xiaoqun Wang, J. Gong, Roberto Battiston, Carlos Díaz, W. De Boer, Liqiu Wang, Pier-Giorgio Rancoita, H. Wu, C Zheng, M. Paniccia, S. Chouridou, M. Bourquin, Andrei Kounine, Q. Yan, F. Giovacchini, L. Quadrani, V Vagelli, M. Vecchi, P. Mott, B. Borgia, W Xu, Andrea Contin, Luísa Arruda, H. D. Phan, F. Zhao, G. Coignet, A. Rozhkov, Zhixiang Tang, C. H. Chung, J Tian, M. Vazquez Acosta, C X Wang, Zhen Sun, Yung Huang Chang, K. Luebelsmeyer, D. Rozza, Bernd Heber, R. Q. Xiong, A. Eline, N. Zimmermann, M. Pauluzzi, K. C. Han, J. H. Zhang, J. Q. Li, L. Wang, Q. L. Wang, Mayda Velasco, M. Behlmann, Yi-Cong Yu, A. Lebedev, S. Q. Lu, A. Kuhlman, V. Formato, Varlen Grabski, S Wang, C. Delgado, G. Martinez, G. La Vacca, F. Dimiccoli, Zheng Wang, H. L. Zhuang, Ignazio Lazzizzera, R. Sonnabend, Valery Zhukov, M. Graziani, G. Laurenti, Y. Yang, A. Reina Conde, J Liang, B. Beischer, Jun Liu, J. D. Burger, E F Bueno, R Piandani, Z. H. He, David Maurin, V. Choutko, D M Gómez-Coral, F. Barao, Yu. Galaktionov, H. Jinchi, S. Schael, R. J. García-López, A. Kulemzin, C. Consolandi, G. Ambrosi, C. Gámez, M. Palermo, Timothy H. Hsieh, H. Yi, F. Machate, H. Y. Chou, T. Siedenburg, F. Nozzoli, Corrado Gargiulo, C. Light, N. Nikonov, T. Martin, J. W. Song, M. Duranti, H. T. Lee, Elisa Laudi, R. K. Hashmani, J. Berdugo, J H Li, J Negrete, Mario Zannoni, S. Li, A. Pashnin, Z. Cui, V. Di Felice, Laurent Derome, J. Casaus, D. Grandi, S. Di Falco, P. von Doetinchem, Xi Luo, K. Kanishev, Claudio Corti, X. D. Cai, T. Urban, Thomas Lippert, Henning Gast, B. Bertucci, Nicola Tomassetti, L. Ali Cavasonza, S. C. Lee, K. Bollweg, Qie Sun, L Strigari, C. Solano, F. Donnini, Lin Cheng, S. Burmeister, C. Freeman, P. H. Fisher, X J Song, Massimo Gervasi, Ilya Usoskin, Samuel C.C. Ting, B. Khiali, J. Z. Luo, M Valencia-Otero, W. J. Burger, S. Başeğmez-du Pree, A. Bartoloni, F. Cervelli, G R Chen, M. Incagli, K. Dadzie, M. Capell, J. Marquardt, Behcet Alpat, D. C. Mo, Matteo Boschini, Roald Z. Sagdeev, Yu Wang, X. W. Tang, F. Palmonari, M. Aguilar, S. Della Torre, S. Rosier-Lees, J. P. Vialle, C. Mañá, Fajun Zhang, Veronica Bindi, M. Molero, Z. M. Zheng, T. Kirn, Jonathan L. Feng, M S Allen, Q. Meng, E. Valente, Chuanguo Zhang, Sadakazu Haino, C. Tüysüz, N. Masi, L. Barrin, A. Schulz von Dratzig, A. Zichichi, T Su, V. V. Mikhailov, Stepan Poluianov, Z. Q. Yu, F. Dong, Y. Chen, Z Liu, Z. L. Weng, D. Rapin, V. Plyaskin, Mauro Tacconi, B. S. Shan, M. B. Demirköz, Yi Jia, L Mussolin, Corinne Goy, 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), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), AMS, Aguilar M., Cavasonza L.A., Allen M.S., Alpat B., Ambrosi G., Arruda L., Attig N., Barao F., Barrin L., Bartoloni A., Basegmez-Du Pree S., Battiston R., Behlmann M., Beischer B., Berdugo J., Bertucci B., Bindi V., De Boer W., Bollweg K., Borgia B., Boschini M.J., Bourquin M., Bueno E.F., Burger J., Burger W.J., Burmeister S., Cai X.D., Capell M., Casaus J., Castellini G., Cervelli F., Chang Y.H., Chen G.M., Chen G.R., Chen H.S., Chen Y., Cheng L., Chou H.Y., Chouridou S., Choutko V., Chung C.H., Clark C., Coignet G., Consolandi C., Contin A., Corti C., Cui Z., Dadzie K., Delgado C., Della Torre S., Demirkoz M.B., Derome L., Di Falco S., Di Felice V., Diaz C., Dimiccoli F., Von Doetinchem P., Dong F., Donnini F., Duranti M., Egorov A., Eline A., Feng J., Fiandrini E., Fisher P., Formato V., Freeman C., Galaktionov Y., Gamez C., Garcia-Lopez R.J., Gargiulo C., Gast H., Gervasi M., Giovacchini F., Gomez-Coral D.M., Gong J., Goy C., Grabski V., Grandi D., Graziani M., Haino S., Han K.C., Hashmani R.K., He Z.H., Heber B., Hsieh T.H., Hu J.Y., Incagli M., Jang W.Y., Jia Y., Jinchi H., Kanishev K., Khiali B., Kim G.N., Kirn T., Konyushikhin M., Kounina O., Kounine A., Koutsenko V., Kuhlman A., Kulemzin A., La Vacca G., Laudi E., Laurenti G., Lazzizzera I., Lebedev A., Lee H.T., Lee S.C., Li J.Q., Li M., Li Q., Li S., Li J.H., Li Z.H., Liang J., Light C., Lin C.H., Lippert T., Liu J.H., Liu Z., Lu S.Q., Lu Y.S., Luebelsmeyer K., Luo J.Z., Luo X., Lyu S.S., Machate F., Mana C., Marin J., Marquardt J., Martin T., Martinez G., Masi N., Maurin D., Menchaca-Rocha A., Meng Q., Mikhailov V.V., Mo D.C., Molero M., Mott P., Mussolin L., Negrete J., Nikonov N., Nozzoli F., Oliva A., Orcinha M., Palermo M., Palmonari F., Paniccia M., Pashnin A., Pauluzzi M., Pensotti S., Phan H.D., Piandani R., Plyaskin V., Poluianov S., Qin X., Qu Z.Y., Quadrani L., Rancoita P.G., Rapin D., Conde A.R., Robyn E., Rosier-Lees S., Rozhkov A., Rozza D., Sagdeev R., Schael S., Von Dratzig A.S., Schwering G., Seo E.S., Shakfa Z., Shan B.S., Siedenburg T., Solano C., Song J.W., Song X.J., Sonnabend R., Strigari L., Su T., Sun Q., Sun Z.T., Tacconi M., Tang X.W., Tang Z.C., Tian J., Ting S.C.C., Ting S.M., Tomassetti N., Torsti J., Tuysuz C., Urban T., Usoskin I., Vagelli V., Vainio R., Valencia-Otero M., Valente E., Valtonen E., Vazquez Acosta M., Vecchi M., Velasco M., Vialle J.P., Wang C.X., Wang L., Wang L.Q., Wang N.H., Wang Q.L., Wang S., Wang X., Wang Y., Wang Z.M., Wei J., Weng Z.L., Wu H., Xiong R.Q., Xu W., Yan Q., Yang Y., Yashin I.I., Yi H., Yu Y.M., Yu Z.Q., Zannoni M., Zhang C., Zhang F., Zhang F.Z., Zhang J.H., Zhang Z., Zhao F., Zheng C., Zheng Z.M., Zhuang H.L., Zhukov V., Zichichi A., Zimmermann N., Zuccon P., Bourquin, Maurice, Chen, Yao, Liu, Zhen, Paniccia, Mercedes, Rapin, Divic Jean, Robyn, Erwan, Wei, Jiahui, Astronomy, Aguilar, M, Cavasonza, L, Allen, M, Alpat, B, Ambrosi, G, Arruda, L, Attig, N, Barao, F, Barrin, L, Bartoloni, A, Başeğmez-du Pree, S, Battiston, R, Behlmann, M, Beischer, B, Berdugo, J, Bertucci, B, Bindi, V, de Boer, W, Bollweg, K, Borgia, B, Boschini, M, Bourquin, M, Bueno, E, Burger, J, Burger, W, Burmeister, S, Cai, X, Capell, M, Casaus, J, Castellini, G, Cervelli, F, Chang, Y, Chen, G, Chen, H, Chen, Y, Cheng, L, Chou, H, Chouridou, S, Choutko, V, Chung, C, Clark, C, Coignet, G, Consolandi, C, Contin, A, Corti, C, Cui, Z, Dadzie, K, Delgado, C, Della Torre, S, Demirköz, M, Derome, L, Di Falco, S, Di Felice, V, Díaz, C, Dimiccoli, F, von Doetinchem, P, Dong, F, Donnini, F, Duranti, M, Egorov, A, Eline, A, Feng, J, Fiandrini, E, Fisher, P, Formato, V, Freeman, C, Galaktionov, Y, Gámez, C, García-López, R, Gargiulo, C, Gast, H, Gervasi, M, Giovacchini, F, Gómez-Coral, D, Gong, J, Goy, C, Grabski, V, Grandi, D, Graziani, M, Haino, S, Han, K, Hashmani, R, He, Z, Heber, B, Hsieh, T, Hu, J, Incagli, M, Jang, W, Jia, Y, Jinchi, H, Kanishev, K, Khiali, B, Kim, G, Kirn, T, Konyushikhin, M, Kounina, O, Kounine, A, Koutsenko, V, Kuhlman, A, Kulemzin, A, La Vacca, G, Laudi, E, Laurenti, G, Lazzizzera, I, Lebedev, A, Lee, H, Lee, S, Li, J, Li, M, Li, Q, Li, S, Li, Z, Liang, J, Light, C, Lin, C, Lippert, T, Liu, J, Liu, Z, Lu, S, Lu, Y, Luebelsmeyer, K, Luo, J, Luo, X, Lyu, S, Machate, F, Mañá, C, Marín, J, Marquardt, J, Martin, T, Martínez, G, Masi, N, Maurin, D, Menchaca-Rocha, A, Meng, Q, Mikhailov, V, Mo, D, Molero, M, Mott, P, Mussolin, L, Negrete, J, Nikonov, N, Nozzoli, F, Oliva, A, Orcinha, M, Palermo, M, Palmonari, F, Paniccia, M, Pashnin, A, Pauluzzi, M, Pensotti, S, Phan, H, Piandani, R, Plyaskin, V, Poluianov, S, Qin, X, Qu, Z, Quadrani, L, Rancoita, P, Rapin, D, Conde, A, Robyn, E, Rosier-Lees, S, Rozhkov, A, Rozza, D, Sagdeev, R, Schael, S, von Dratzig, A, Schwering, G, Seo, E, Shakfa, Z, Shan, B, Siedenburg, T, Solano, C, Song, J, Song, X, Sonnabend, R, Strigari, L, Su, T, Sun, Q, Sun, Z, Tacconi, M, Tang, X, Tang, Z, Tian, J, Ting, S, Tomassetti, N, Torsti, J, Tüysüz, C, Urban, T, Usoskin, I, Vagelli, V, Vainio, R, Valencia-Otero, M, Valente, E, Valtonen, E, Vázquez Acosta, M, Vecchi, M, Velasco, M, Vialle, J, Wang, C, Wang, L, Wang, N, Wang, Q, Wang, S, Wang, X, Wang, Y, Wang, Z, Wei, J, Weng, Z, Wu, H, Xiong, R, Xu, W, Yan, Q, Yang, Y, Yashin, I, Yi, H, Yu, Y, Yu, Z, Zannoni, M, Zhang, C, Zhang, F, Zhang, J, Zhang, Z, Zhao, F, Zheng, C, Zheng, Z, Zhuang, H, Zhukov, V, Zichichi, A, Zimmermann, N, and Zuccon, P
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Cosmic ray composition & spectra ,General Physics and Astronomy ,Iron nuclei ,primary [cosmic radiation] ,Astrophysics ,Cosmic ray iron ,iron: nucleus ,7. Clean energy ,International Space Station ,01 natural sciences ,GALACTIC COSMIC RAYS, ALPHA MAGNETIC SPECTROMETER, INTERNATIONAL SPACE STATION ,ALPHA MAGNETIC SPECTROMETER ,Rigidity (electromagnetism) ,Cosmology & Astrophysics ,Primary (astronomy) ,Alpha Magnetic Spectrometer ,INTERNATIONAL SPACE STATION ,AMS ,Detectors and Experimental Techniques ,Physics ,Range (particle radiation) ,ratio [flux] ,Cosmic rays & astroparticles ,FIS/01 - FISICA SPERIMENTALE ,Cosmic ray propagation ,Sapce detectors ,Alpha magnetic Spectrometer ,Gravitation ,Astrophysics and Astronomy ,Astrophysics::High Energy Astrophysical Phenomena ,satellite ,Rigidity (psychology) ,Cosmic ray ,ddc:500.2 ,helium ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Gravitation and Astrophysics ,Cosmic ray acceleration ,FIS/05 - ASTRONOMIA E ASTROFISICA ,Flux (metallurgy) ,cosmic rays ,0103 physical sciences ,Cosmic ray nuclei ,ddc:530 ,[PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det] ,Cosmic Rays, Iron nuclei, Alpha Magnetic Spectrometer ,010306 general physics ,Cosmic rays ,GALACTIC COSMIC RAYS ,AMS Collaboration ,ISS ,carbon ,Cosmic ray sources ,magnetic spectrometer ,Flux ratio ,flux: ratio ,Cosmic ray physics ,cosmic radiation: primary ,13. Climate action ,nucleus [iron] ,AMS Collaboration, Cosmic ray acceleration, Cosmic ray composition & spectra, Cosmic ray propagation, Cosmic ray sources, Cosmic rays & astroparticles, Gravitation, Cosmology & Astrophysics ,Astroparticle physics ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,oxygen - Abstract
Physical review letters 126(4), 041104 (2021). doi:10.1103/PhysRevLett.126.041104, Published by APS, College Park, Md.
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- 2021
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- View/download PDF
8. Properties of Heavy Secondary Fluorine Cosmic Rays: Results from the Alpha Magnetic Spectrometer
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Jun Hu, Yu. Galaktionov, A. Rozhkov, C. H. Chung, W Xu, Luísa Arruda, D M Gómez-Coral, M. Behlmann, L Mussolin, M. Konyushikhin, Z. Y. Qu, H. T. Lee, Corinne Goy, Q. Meng, C. Gámez, Eun-Suk Seo, Ying Lu, Valery Zhukov, A. Lebedev, A. Kuhlman, Mario Zannoni, Rami Vainio, P. Zuccon, A. Menchaca-Rocha, A.I. Oliva, V. Koutsenko, Eino Valtonen, V. Formato, Varlen Grabski, Sadakazu Haino, C. Tüysüz, G. Schwering, E Robyn, T. Urban, J. D. Burger, Corrado Gargiulo, Jonathan L. Feng, Fan Zhang, Z Liu, T. Siedenburg, H. D. Phan, M Valencia-Otero, W. J. Burger, F. Giovacchini, F. Zhao, Z. H. Li, Qiang Li, Z. L. Weng, D. Rapin, V. Plyaskin, P. von Doetinchem, X. D. Cai, A. Kulemzin, P. Mott, Pier-Giorgio Rancoita, M S Allen, Liqiu Wang, A. Reina Conde, J Liang, I. I. Yashin, Mauro Tacconi, S. Schael, Zhixiang Tang, R. K. Hashmani, G. N. Kim, Zhihua Zhang, C. Clark, S. S. Lyu, J Negrete, B. S. Shan, M. B. Demirköz, F. Cervelli, Timothy H. Hsieh, Zhen Sun, Claudio Corti, H. Yi, L Strigari, B. Khiali, J. Q. Li, Z. Q. Yu, G. La Vacca, Yi Jia, David Maurin, K. C. Han, Xi Luo, F. Donnini, S. C. Lee, M. Vazquez Acosta, C X Wang, F. Dong, Laurent Derome, Elisa Laudi, J Wei, Yung Huang Chang, Q. L. Wang, D. C. Mo, Massimo Gervasi, K. Luebelsmeyer, A. Eline, C Zheng, L. Ali Cavasonza, S Wang, Ilya Usoskin, C. Delgado, J. Z. Luo, Henning Gast, Lucio Quadrani, Zheng Wang, M. Paniccia, M. Capell, R. Sonnabend, J. Marquardt, G. Martinez, Julio C. Marín, M. Li, J. Berdugo, M. Graziani, M. Incagli, V. Choutko, G. Ambrosi, J H Li, C. Consolandi, S. Burmeister, J. J. Torsti, S. Pensotti, S. M. Ting, J Tian, X J Song, A. Pashnin, K. Dadzie, M. Bourquin, S. Li, R. J. García-López, Naihua Wang, A. Bartoloni, S. Di Falco, Fajun Zhang, E. Fiandrini, E F Bueno, W. Y. Jang, R Piandani, Bernd Heber, H. S. Chen, R. Q. Xiong, S. Chouridou, Guo-Ming Chen, H. Jinchi, Mayda Velasco, Chia-Hui Lin, N. Attig, S. Başeğmez-du Pree, D. Grandi, K. Bollweg, J. Gong, Qie Sun, C. Solano, B. Bertucci, Roald Z. Sagdeev, S. Q. Lu, S. Della Torre, Andrei Kounine, S. Rosier-Lees, Q. Yan, H. L. Zhuang, Xiaoqun Wang, Y. Chen, G. Castellini, G R Chen, E. Valente, X. Qin, Chuanguo Zhang, Yi-Cong Yu, Y. Yang, F. Machate, M. Orcinha, M. Vecchi, H. Y. Chou, M. Pauluzzi, N. Nikonov, T. Martin, J. W. Song, M. Duranti, Z. Cui, N. Masi, L. Barrin, A. Schulz von Dratzig, A. Zichichi, Yu Wang, J. Casaus, T Su, V. V. Mikhailov, Stepan Poluianov, M. Aguilar, Lin Cheng, V Vagelli, Jun Liu, Z. H. He, F. Nozzoli, V. Di Felice, L. Wang, J. H. Zhang, C. Freeman, Samuel C.C. Ting, B Beranek, Matteo Boschini, A. Egorov, Z Shakfa, Carlos Díaz, D. Rozza, G. Laurenti, M. Palermo, Roberto Battiston, B. Borgia, Ignazio Lazzizzera, C. Mañá, Veronica Bindi, M. Molero, T. Kirn, O. Kounina, H. Wu, Andrea Contin, G. Coignet, F. Dimiccoli, F. Barao, Thomas Lippert, P. H. Fisher, F. Palmonari, X. W. Tang, J. P. Vialle, Z. M. Zheng, C. Light, K. Kanishev, Nicola Tomassetti, Behcet Alpat, 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), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), AMS, Bourquin, Maurice, Chen, Yao, Liu, Zhen, Paniccia, Mercedes, Rapin, Divic Jean, Robyn, Erwan, Wei, Jiahui, Astronomy, Aguilar M., Cavasonza L.A., Allen M.S., Alpat B., Ambrosi G., Arruda L., Attig N., Barao F., Barrin L., Bartoloni A., Basegmez-Du Pree S., Battiston R., Behlmann M., Beranek B., Berdugo J., Bertucci B., Bindi V., Bollweg K., Borgia B., Boschini M.J., Bourquin M., Bueno E.F., Burger J., Burger W.J., Burmeister S., Cai X.D., Capell M., Casaus J., Castellini G., Cervelli F., Chang Y.H., Chen G.M., Chen G.R., Chen H.S., Chen Y., Cheng L., Chou H.Y., Chouridou S., Choutko V., Chung C.H., Clark C., Coignet G., Consolandi C., Contin A., Corti C., Cui Z., Dadzie K., Delgado C., Della Torre S., Demirkoz M.B., Derome L., Di Falco S., Di Felice V., Diaz C., Dimiccoli F., Von Doetinchem P., Dong F., Donnini F., Duranti M., Egorov A., Eline A., Feng J., Fiandrini E., Fisher P., Formato V., Freeman C., Galaktionov Y., Gamez C., Garcia-Lopez R.J., Gargiulo C., Gast H., Gervasi M., Giovacchini F., Gomez-Coral D.M., Gong J., Goy C., Grabski V., Grandi D., Graziani M., Haino S., Han K.C., Hashmani R.K., He Z.H., Heber B., Hsieh T.H., Hu J.Y., Incagli M., Jang W.Y., Jia Y., Jinchi H., Kanishev K., Khiali B., Kim G.N., Kirn T., Konyushikhin M., Kounina O., Kounine A., Koutsenko V., Kuhlman A., Kulemzin A., La Vacca G., Laudi E., Laurenti G., Lazzizzera I., Lebedev A., Lee H.T., Lee S.C., Li J.Q., Li M., Li Q., Li S., Li J.H., Li Z.H., Liang J., Light C., Lin C.H., Lippert T., Liu J.H., Liu Z., Lu S.Q., Lu Y.S., Luebelsmeyer K., Luo J.Z., Luo X., Lyu S.S., Machate F., Mana C., Marin J., Marquardt J., Martin T., Martinez G., Masi N., Maurin D., Menchaca-Rocha A., Meng Q., Mikhailov V.V., Mo D.C., Molero M., Mott P., Mussolin L., Negrete J., Nikonov N., Nozzoli F., Oliva A., Orcinha M., Palermo M., Palmonari F., Paniccia M., Pashnin A., Pauluzzi M., Pensotti S., Phan H.D., Piandani R., Plyaskin V., Poluianov S., Qin X., Qu Z.Y., Quadrani L., Rancoita P.G., Rapin D., Conde A.R., Robyn E., Rosier-Lees S., Rozhkov A., Rozza D., Sagdeev R., Schael S., Schulz Von Dratzig A., Schwering G., Seo E.S., Shakfa Z., Shan B.S., Siedenburg T., Solano C., Song J.W., Song X.J., Sonnabend R., Strigari L., Su T., Sun Q., Sun Z.T., Tacconi M., Tang X.W., Tang Z.C., Tian J., Ting S.C.C., Ting S.M., Tomassetti N., Torsti J., Tuysuz C., Urban T., Usoskin I., Vagelli V., Vainio R., Valencia-Otero M., Valente E., Valtonen E., Vazquez Acosta M., Vecchi M., Velasco M., Vialle J.P., Wang C.X., Wang L., Wang L.Q., Wang N.H., Wang Q.L., Wang S., Wang X., Wang Y., Wang Z.M., Wei J., Weng Z.L., Wu H., Xiong R.Q., Xu W., Yan Q., Yang Y., Yashin I.I., Yi H., Yu Y.M., Yu Z.Q., Zannoni M., Zhang C., Zhang F., Zhang F.Z., Zhang J.H., Zhang Z., Zhao F., Zheng C., Zheng Z.M., Zhuang H.L., Zhukov V., Zichichi A., Zuccon P., Aguilar, M, Cavasonza, L, Allen, M, Alpat, B, Ambrosi, G, Arruda, L, Attig, N, Barao, F, Barrin, L, Bartoloni, A, Başeğmez-du Pree, S, Battiston, R, Behlmann, M, Beranek, B, Berdugo, J, Bertucci, B, Bindi, V, Bollweg, K, Borgia, B, Boschini, M, Bourquin, M, Bueno, E, Burger, J, Burger, W, Burmeister, S, Cai, X, Capell, M, Casaus, J, Castellini, G, Cervelli, F, Chang, Y, Chen, G, Chen, H, Chen, Y, Cheng, L, Chou, H, Chouridou, S, Choutko, V, Chung, C, Clark, C, Coignet, G, Consolandi, C, Contin, A, Corti, C, Cui, Z, Dadzie, K, Delgado, C, Della Torre, S, Demirköz, M, Derome, L, Di Falco, S, Di Felice, V, Díaz, C, Dimiccoli, F, von Doetinchem, P, Dong, F, Donnini, F, Duranti, M, Egorov, A, Eline, A, Feng, J, Fiandrini, E, Fisher, P, Formato, V, Freeman, C, Galaktionov, Y, Gámez, C, García-López, R, Gargiulo, C, Gast, H, Gervasi, M, Giovacchini, F, Gómez-Coral, D, Gong, J, Goy, C, Grabski, V, Grandi, D, Graziani, M, Haino, S, Han, K, Hashmani, R, He, Z, Heber, B, Hsieh, T, Hu, J, Incagli, M, Jang, W, Jia, Y, Jinchi, H, Kanishev, K, Khiali, B, Kim, G, Kirn, T, Konyushikhin, M, Kounina, O, Kounine, A, Koutsenko, V, Kuhlman, A, Kulemzin, A, La Vacca, G, Laudi, E, Laurenti, G, Lazzizzera, I, Lebedev, A, Lee, H, Lee, S, Li, J, Li, M, Li, Q, Li, S, Li, Z, Liang, J, Light, C, Lin, C, Lippert, T, Liu, J, Liu, Z, Lu, S, Lu, Y, Luebelsmeyer, K, Luo, J, Luo, X, Lyu, S, Machate, F, Mañá, C, Marín, J, Marquardt, J, Martin, T, Martínez, G, Masi, N, Maurin, D, Menchaca-Rocha, A, Meng, Q, Mikhailov, V, Mo, D, Molero, M, Mott, P, Mussolin, L, Negrete, J, Nikonov, N, Nozzoli, F, Oliva, A, Orcinha, M, Palermo, M, Palmonari, F, Paniccia, M, Pashnin, A, Pauluzzi, M, Pensotti, S, Phan, H, Piandani, R, Plyaskin, V, Poluianov, S, Qin, X, Qu, Z, Quadrani, L, Rancoita, P, Rapin, D, Conde, A, Robyn, E, Rosier-Lees, S, Rozhkov, A, Rozza, D, Sagdeev, R, Schael, S, Schulz von Dratzig, A, Schwering, G, Seo, E, Shakfa, Z, Shan, B, Siedenburg, T, Solano, C, Song, J, Song, X, Sonnabend, R, Strigari, L, Su, T, Sun, Q, Sun, Z, Tacconi, M, Tang, X, Tang, Z, Tian, J, Ting, S, Tomassetti, N, Torsti, J, Tüysüz, C, Urban, T, Usoskin, I, Vagelli, V, Vainio, R, Valencia-Otero, M, Valente, E, Valtonen, E, Vázquez Acosta, M, Vecchi, M, Velasco, M, Vialle, J, Wang, C, Wang, L, Wang, N, Wang, Q, Wang, S, Wang, X, Wang, Y, Wang, Z, Wei, J, Weng, Z, Wu, H, Xiong, R, Xu, W, Yan, Q, Yang, Y, Yashin, I, Yi, H, Yu, Y, Yu, Z, Zannoni, M, Zhang, C, Zhang, F, Zhang, J, Zhang, Z, Zhao, F, Zheng, C, Zheng, Z, Zhuang, H, Zhukov, V, Zichichi, A, and Zuccon, P
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General Physics and Astronomy ,Galactic cosmic rays ,01 natural sciences ,Power law ,Rigidity (electromagnetism) ,Alpha magnetic spectrometer ,Alpha Magnetic Spectrometer ,AMS ,Physics ,Range (particle radiation) ,cosmic radiation: propagation ,Galactic cosmic rays, AMS ,ratio [flux] ,secondary [cosmic radiation] ,Cosmic ray flux ,Flux ratio ,3. Good health ,Cosmic ray propagation ,Astrophysics and Astronomy ,Astrophysics::High Energy Astrophysical Phenomena ,satellite ,chemistry.chemical_element ,Cosmic ray ,ddc:500.2 ,Astrophysics::Cosmology and Extragalactic Astrophysics ,helium ,Gravitation and Astrophysics ,Nuclear physics ,FIS/05 - ASTRONOMIA E ASTROFISICA ,Flux (metallurgy) ,fluorine ,0103 physical sciences ,spectra, Cosmic ray propagation, Cosmic ray sources, Cosmic rays & ,Cosmic ray composition & ,ddc:530 ,010306 general physics ,cosmic radiation: secondary ,Alpha magnetic spectrometer experiment ,Power-law ,International Space station ,magnetic spectrometer ,flux: ratio ,Automatic Keywords ,chemistry ,Propagation properties ,Fluorine ,propagation [cosmic radiation] ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,oxygen ,astroparticles, Particle astrophysic - Abstract
International audience; Precise knowledge of the charge and rigidity dependence of the secondary cosmic ray fluxes and the secondary-to-primary flux ratios is essential in the understanding of cosmic ray propagation. We report the properties of heavy secondary cosmic ray fluorine F in the rigidity $R$ range 2.15 GV to 2.9 TV based on 0.29 million events collected by the Alpha Magnetic Spectrometer experiment on the International Space Station. The fluorine spectrum deviates from a single power law above 200 GV. The heavier secondary-to-primary F/Si flux ratio rigidity dependence is distinctly different from the lighter B/O (or B/C) rigidity dependence. In particular, above 10 GV, the $^{\textrm{F/Si}}_{\textrm{B/O}}$ ratio can be described by a power law $R^δ$ with $δ=0.052±0.007$. This shows that the propagation properties of heavy cosmic rays, from F to Si, are different from those of light cosmic rays, from He to O, and that the secondary cosmic rays have two classes.
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- 2021
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9. Solar Intensity X-Ray and Particle Spectrometer SIXS: Instrument Design and First Results
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Tatsuaki Okada, Monica Laurenza, Hans Andersson, Rami Vainio, Adrian Martindale, Walter Schmidt, Juhani Huovelin, Anna Milillo, J. Lehti, T. Vihavainen, Manuel Grande, Emilia Kilpua, J. Peltonen, Shyama Narendranath, Philipp Oleynik, Karri Muinonen, Jussi Saari, Erkka Heino, A. Lehtolainen, S. Korpela, Riku Jarvinen, Eero Esko, Eino Valtonen, Emma J. Bunce, M. Talvioja, P. Portin, Maria Genzer, S. Nenonen, University of Helsinki, University of Turku, University of Leicester, Aberystwyth University, Oxford Instruments Group Plc, ASRO - Aboa Space Research Oy, Finnish Meteorological Institute, Space Systems Finland Oy, Talvioja Consulting Oy, Patria Aviation, Indian Space Research Organization, Tuija Pulkkinen Group, JAXA Institute of Space and Astronautical Science, INAF - Osservatorio Astronomico di Roma, INAF, Osservatorio Astronomico di Roma, Department of Electronics and Nanoengineering, Aalto-yliopisto, and Aalto University
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Solar System ,010504 meteorology & atmospheric sciences ,Astrophysics::High Energy Astrophysical Phenomena ,BepiColombo ,Electrons ,Solar corona ,Space weather ,7. Clean energy ,01 natural sciences ,Planet ,0103 physical sciences ,Interplanetary magnetic field ,010303 astronomy & astrophysics ,Instrumentation ,0105 earth and related environmental sciences ,Physics ,Spectrometer ,Solar energetic particles ,Solar X-rays ,Astronomy ,Astronomy and Astrophysics ,Corona ,13. Climate action ,Space and Planetary Science ,Physics::Space Physics ,Planet Mercury ,Astrophysics::Earth and Planetary Astrophysics ,Protons ,Exosphere - Abstract
The Solar Intensity X-ray and particle Spectrometer (SIXS) on the BepiColombo Mercury Planetary Orbiter (“Bepi”) measures the direct solar X-rays, energetic protons, and electrons that bombard, and interact with, the Hermean surface. The interactions result in X-ray fluorescence and scattering, and particle induced X-ray emission (PIXE), i.e. “glow” of the surface in X-rays. Simultaneous monitoring of the incident and emitted radiation enables derivation of the abundances of some chemical elements and scattering properties of the outermost surface layer of the planet, and it may reveal other sources of X-ray emission, due to, for example, weak aurora-like phenomena in Mercury’s exosphere. Mapping of the Hermean X-ray emission is the main task of the MIXS instrument onboard BepiColombo. SIXS data will also be used for investigations of the solar X-ray corona and solar energetic particles (SEP), both in the cruise phase and the passes of the Earth, Venus and Mercury before the arrival at Mercury’s orbit, and the final science phase at Mercury’s orbit. These observations provide the first-ever opportunity for in-situ measurements of the propagation of SEPs, their interactions with the interplanetary magnetic field, and space weather phenomena in multiple locations throughout the inner solar system far away from the Earth, and more extensively at Mercury’s orbit.In this paper we describe the scientific objectives, design and calibrations, operational principles, and scientific performance of the final SIXS instrument launched to the mission to planet Mercury onboard BepiColombo. We also provide the first analysis results of science observations with SIXS, that were made during the Near-Earth Commissioning Phase and early cruise phase operations in 2018–19, including the background X-ray sky observations and “first light” observations of the Sun with the SIXS X-ray detection system (SIXS-X), and in-situ energetic electron and proton observations with the SIXS Particle detection system (SIXS-P).
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- 2020
10. Calibration of RADMON radiation monitor onboard Aalto-1 CubeSat
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Risto Punkkinen, Edward Hæggström, Eino Valtonen, Rami Vainio, Jaan Praks, Heli Hietala, Hannu-Pekka Hedman, Philipp Oleynik, J. Peltonen, Petri Niemelä, Jan Gieseler, Oleksiy Dudnik, Tero Säntti, Arttu Punkkinen, University of Turku, NASU - Institute of Radio Astronomy, University of Helsinki, Department of Electronics and Nanoengineering, Aalto-yliopisto, Aalto University, and Department of Physics
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Atmospheric Science ,CubeSats ,Solar energetic particles ,Physics - Instrumentation and Detectors ,010504 meteorology & atmospheric sciences ,Physics::Instrumentation and Detectors ,Aerospace Engineering ,Electron precipitation ,SCINTILLATION PROCESS ,FOS: Physical sciences ,Radiation ,Scintillator ,01 natural sciences ,7. Clean energy ,symbols.namesake ,0103 physical sciences ,Calibration ,SPECTRA ,CubeSat ,010303 astronomy & astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,0105 earth and related environmental sciences ,Remote sensing ,Physics ,Detector ,Astrophysics::Instrumentation and Methods for Astrophysics ,NANOSATELLITE ,Astronomy and Astrophysics ,Instrumentation and Detectors (physics.ins-det) ,115 Astronomy, Space science ,Radiation belts ,Geophysics ,Space and Planetary Science ,CSI(TL) ,Van Allen radiation belt ,SIMULATION ,symbols ,General Earth and Planetary Sciences ,PARTICLE IDENTIFICATION ,Astrophysics - Instrumentation and Methods for Astrophysics ,Energy (signal processing) - Abstract
RADMON is a small radiation monitor designed and assembled by students of the University of Turku and the University of Helsinki. It is flown on-board Aalto-1, a 3-unit CubeSat in low Earth orbit at about 500 km altitude. The detector unit of the instrument consists of two detectors, a Si solid-state detector and a CsI(Tl) scintillator, and utilizes the \textDelta{E}-E technique to determine the total energy and species of each particle hitting the detector. We present the results of the on-ground and in-flight calibration campaigns of the instrument, as well as the characterization of its response through extensive simulations within the Geant4 framework. The overall energy calibration margin achieved is about 5\%. The full instrument response to protons and electrons is presented and the issue of proton contamination of the electron channels is quantified and discussed., Comment: 27 pages, 9 figures
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- 2020
11. Properties of High-Energy Solar Particle Events Associated with Solar Radio Emissions
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Dheyaa Ameri, Silja Pohjolainen, and Eino Valtonen
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Physics ,010504 meteorology & atmospheric sciences ,Solar flare ,Proton ,Velocity dispersion ,Astronomy and Astrophysics ,Astrophysics ,Electron ,01 natural sciences ,Spectral line ,Wavelength ,Path length ,Space and Planetary Science ,0103 physical sciences ,Coronal mass ejection ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences - Abstract
We have analysed 58 high-energy proton events and 36 temporally related near-relativistic electron events from the years 1997 – 2015 for which the velocity dispersion analysis of the first-arriving particles gave the apparent path lengths between 1 and 3 AU. We investigated the dependence of the characteristics of the proton events on the associations of type II, III, and IV radio bursts. We also examined the properties of the soft X-ray flares and coronal mass ejections associated with these events. All proton events were associated with decametric type III radio bursts, while type IV emission was observed only in the meter wavelengths in some of the events (32/58). Almost all proton events (56/58) were associated with radio type II bursts: 11 with metric (m) type II only, 11 with decametric–hectometric (DH) only, and 34 with type II radio bursts at both wavelength ranges. By examining several characteristics of the proton events, we discovered that the proton events can be divided into two categories. The characteristics of events belonging to the same category were similar, while they significantly differed between events in different categories. The distinctive factors between the categories were the wavelength range of the associated type II radio emission and the temporal relation of the proton release with respect to the type II onset. In Category 1 are the events which were associated with only metric type II emission or both m and DH type II and the release time of protons was before the DH type II onset (18/56 events). Category 2 consists of the events which were associated with only DH type II emission or both m and DH type II and the protons were released at or after the DH type II onset (31/56 events). For seven of the 56 events we were not able to determine a definite category due to timing uncertainties. The events in Category 1 had significantly higher intensity rise rates, shorter rise times, lower release heights, and harder energy spectra than Category 2 events. Category 1 events also originated from magnetically well-connected regions and had only small time differences between the proton release times and the type III onsets. The soft X-ray flares for these events had significantly shorter rise times and durations than for Category 2 events. We found 36 electron events temporally related to the proton events, which fulfilled the same path length criterion as the proton events. We compared the release times of protons and electrons at the Sun, and discovered that in 19 of the 36 events protons were released almost simultaneously (within ${\pm}\,7$ ± 7 minutes) with the electrons, in 16 events protons were released later than the electrons, and in one event electrons were released after the protons. The simultaneous proton and electron events and the delayed proton events did not unambiguously fall in the two categories of proton events, although most of the events in which the protons were released after the electrons belonged to Category 2. We conclude that acceleration of protons in Category 1 events occurred low in the corona, either by CME-driven shocks or below the CMEs in solar flares or in CME initiation related processes. It seems plausible that protons in Category 2 events were accelerated by CME-driven shocks high in the solar corona. Large delays of protons with respect to type III onsets in the events where protons were released after the electrons suggest late acceleration or release of protons close to the Sun, but the exact mechanism causing the delay remained unclear.
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- 2019
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12. Towards Understanding the Origin of Cosmic-Ray Positrons
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B. Borgia, C. Consolandi, C. Clark, M. Bourquin, Ignazio Lazzizzera, M Molero, J Vizán, A. Pashnin, J. J. Torsti, S. Pensotti, Antonino Zichichi, S. M. Ting, J Wei, Andrei Kounine, O. Kounina, H. Wu, E. Fiandrini, Jonathan L. Feng, D. C. Mo, T. Urban, Q. Yan, H. S. Chen, R. Q. Xiong, S. Caroff, V. Choutko, N. Zimmermann, C. Solano, M. Pohl, Mayda Velasco, Andrea Contin, G. Coignet, A. Popkow, K. C. Han, Q. L. Wang, Zhao Wang, A. Datta, C. Delgado, Z. H. He, D. M. Gómez-Coral, F. Nozzoli, M. Vazquez Acosta, T. Eronen, H. Yi, Valery Zhukov, C. H. Chung, P. Mott, X. W. Tang, F. Giovacchini, K. Luebelsmeyer, A. Egorov, W. Xu, J. D. Burger, T. Siedenburg, Carlos Díaz, C. Mañá, Veronica Bindi, Valerio Formato, X. M. Qi, Zhixiang Tang, A. Eline, E. Valente, Arturo Alejandro Menchaca-Rocha, W. De Boer, E. F. Bueno, L Mussolin, J. Q. Li, Claudio Corti, T. Kirn, Naihua Wang, S. Schael, J. P. Vialle, H. Jinchi, M. Behlmann, H. D. Phan, F. Zhao, P. von Doetinchem, X. D. Cai, J. Y. Shi, D. Rozza, Chuanguo Zhang, M. Orcinha, Z. Y. Qu, Henning Gast, F. Barao, Elisa Laudi, Zhen Sun, U. Becker, Frank Liu, M. Graziani, S. Başeğmez-du Pree, Y. J. Yu, F. Donnini, N. Attig, Corinne Goy, Z. M. Zheng, Samuel C.C. Ting, Massimo Gervasi, S. M. Schmidt, G. La Vacca, T. J. N. Nelson, Thomas Lippert, J. H. Zhang, David Maurin, M. Crispoltoni, P. H. Fisher, A. Rozhkov, Matthias Heil, Mario Zannoni, D. Grandi, G. Laurenti, N. Nikonov, J. W. Song, Laurent Derome, Roald Z. Sagdeev, G. Ambrosi, P. G. Rancoita, S. Di Falco, V. Poireau, C. Konak, M. Duranti, S. Della Torre, T. X. Li, Varlen Grabski, F. Palmonari, H. P. Huang, A. Kulemzin, A. Reina Conde, M. Incagli, N. Masi, F. Luo, L. Barrin, G. Schwering, V Vagelli, Corrado Gargiulo, B. Bertucci, M. Palermo, N. Picot-Clemente, Matteo Boschini, G. Castellini, S. Rosier-Lees, Y. H. Chang, A. Schulz von Dratzig, Z. Q. Yu, K. Dadzie, I. Gebauer, P. Azzarello, Zhiqi Huang, F. Dong, A. Bartoloni, Zhihua Zhang, X. Qin, J. Casaus, Liqiu Wang, K. Bollweg, M. Capell, Guo-Ming Chen, A. Barrau, Chia-Hui Lin, Hu Liu, J. Berdugo, J. Gong, S. C. Lee, A. Bachlechner, Eun-Suk Seo, X. Q. Wang, Ying Lu, B. Khiali, C. Leluc, C. Light, K. Kanishev, Nicola Tomassetti, R. J. García-López, M. Vecchi, P. Zuccon, V. Koutsenko, Eino Valtonen, Julio C. Marín, M. Aguilar, M. Pauluzzi, Z. H. Li, Qiang Li, Z Liu, Xiaoqun Wang, Yaomin Dai, Y. Chen, K. H. Guo, S. Zeissler, A. Lebedev, Z. L. Weng, D. Rapin, V. Plyaskin, G. Martinez, J. Q. Ni, F. Dimiccoli, F. Machate, H. Y. Chou, Mauro Tacconi, Q. Meng, Z. Cui, Sadakazu Haino, T. Martin, Yang Yang, B. S. Shan, S. Q. Lu, M. B. Demirköz, Lin Cheng, H. L. Zhuang, C. Perrina, L. Basara, Yi Jia, B. Beischer, Fan Zhang, S. S. Lyu, A. Oliva, M. Paniccia, J Tian, Yu. Galaktionov, H. T. Lee, W. J. Burger, F. Cervelli, Timothy H. Hsieh, Xi Luo, L. Quadrani, Luísa Arruda, L. Ali Cavasonza, J. Z. Luo, Roberto Battiston, Aguilar, M, Ali Cavasonza, L, Ambrosi, G, Arruda, L, Attig, N, Azzarello, P, Bachlechner, A, Barao, F, Barrau, A, Barrin, L, Bartoloni, A, Basara, L, Başeğmez-du Pree, S, Battiston, R, Becker, U, Behlmann, M, Beischer, B, Berdugo, J, Bertucci, B, Bindi, V, de Boer, W, Bollweg, K, Borgia, B, Boschini, M, Bourquin, M, Bueno, E, Burger, J, Burger, W, Cai, X, Capell, M, Caroff, S, Casaus, J, Castellini, G, Cervelli, F, Chang, Y, Chen, G, Chen, H, Chen, Y, Cheng, L, Chou, H, Choutko, V, Chung, C, Clark, C, Coignet, G, Consolandi, C, Contin, A, Corti, C, Crispoltoni, M, Cui, Z, Dadzie, K, Dai, Y, Datta, A, Delgado, C, Della Torre, S, Demirköz, M, Derome, L, Di Falco, S, Dimiccoli, F, Díaz, C, von Doetinchem, P, Dong, F, Donnini, F, Duranti, M, Egorov, A, Eline, A, Eronen, T, Feng, J, Fiandrini, E, Fisher, P, Formato, V, Galaktionov, Y, García-López, R, Gargiulo, C, Gast, H, Gebauer, I, Gervasi, M, Giovacchini, F, Gómez-Coral, D, Gong, J, Goy, C, Grabski, V, Grandi, D, Graziani, M, Guo, K, Haino, S, Han, K, He, Z, Heil, M, Hsieh, T, Huang, H, Huang, Z, Incagli, M, Jia, Y, Jinchi, H, Kanishev, K, Khiali, B, Kirn, T, Konak, C, Kounina, O, Kounine, A, Koutsenko, V, Kulemzin, A, La Vacca, G, Laudi, E, Laurenti, G, Lazzizzera, I, Lebedev, A, Lee, H, Lee, S, Leluc, C, Li, J, Li, Q, Li, T, Li, Z, Light, C, Lin, C, Lippert, T, Liu, F, Liu, H, Liu, Z, Lu, S, Lu, Y, Luebelsmeyer, K, Luo, F, Luo, J, Luo, X, Lyu, S, Machate, F, Mañá, C, Marín, J, Martin, T, Martínez, G, Masi, N, Maurin, D, Menchaca-Rocha, A, Meng, Q, Mo, D, Molero, M, Mott, P, Mussolin, L, Nelson, T, Ni, J, Nikonov, N, Nozzoli, F, Oliva, A, Orcinha, M, Palermo, M, Palmonari, F, Paniccia, M, Pashnin, A, Pauluzzi, M, Pensotti, S, Perrina, C, Phan, H, Picot-Clemente, N, Plyaskin, V, Pohl, M, Poireau, V, Popkow, A, Quadrani, L, Qi, X, Qin, X, Qu, Z, Rancoita, P, Rapin, D, Conde, A, Rosier-Lees, S, Rozhkov, A, Rozza, D, Sagdeev, R, Solano, C, Schael, S, Schmidt, S, Schulz von Dratzig, A, Schwering, G, Seo, E, Shan, B, Shi, J, Siedenburg, T, Song, J, Sun, Z, Tacconi, M, Tang, X, Tang, Z, Tian, J, Ting, S, Tomassetti, N, Torsti, J, Urban, T, Vagelli, V, Valente, E, Valtonen, E, Vázquez Acosta, M, Vecchi, M, Velasco, M, Vialle, J, Vizán, J, Wang, L, Wang, N, Wang, Q, Wang, X, Wang, Z, Wei, J, Weng, Z, Wu, H, Xiong, R, Xu, W, Yan, Q, Yang, Y, Yi, H, Yu, Y, Yu, Z, Zannoni, M, Zeissler, S, Zhang, C, Zhang, F, Zhang, J, Zhang, Z, Zhao, F, Zheng, Z, Zhuang, H, Zhukov, V, Zichichi, A, Zimmermann, N, Zuccon, P, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), 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), AMS, Aguilar, M., Ali Cavasonza, L., Ambrosi, G., Arruda, L., Attig, N., Azzarello, P., Bachlechner, A., Barao, F., Barrau, A., Barrin, L., Bartoloni, A., Basara, L., Başeǧmez-Du Pree, S., Battiston, R., Becker, U., Behlmann, M., Beischer, B., Berdugo, J., Bertucci, B., Bindi, V., De Boer, W., Bollweg, K., Borgia, B., Boschini, M.J., Bourquin, M., Bueno, E.F., Burger, J., Burger, W.J., Cai, X.D., Capell, M., Caroff, S., Casaus, J., Castellini, G., Cervelli, F., Chang, Y.H., Chen, G.M., Chen, H.S., Chen, Y., Cheng, L., Chou, H.Y., Choutko, V., Chung, C.H., Clark, C., Coignet, G., Consolandi, C., Contin, A., Corti, C., Crispoltoni, M., Cui, Z., Dadzie, K., Dai, Y.M., Datta, A., Delgado, C., Della Torre, S., Demirköz, M.B., Derome, L., Di Falco, S., Dimiccoli, F., Díaz, C., Von Doetinchem, P., Dong, F., Donnini, F., Duranti, M., Egorov, A., Eline, A., Eronen, T., Feng, J., Fiandrini, E., Fisher, P., Formato, V., Galaktionov, Y., García-López, R.J., Gargiulo, C., Gast, H., Gebauer, I., Gervasi, M., Giovacchini, F., Gómez-Coral, D.M., Gong, J., Goy, C., Grabski, V., Grandi, D., Graziani, M., Guo, K.H., Haino, S., Han, K.C., He, Z.H., Heil, M., Hsieh, T.H., Huang, H., Huang, Z.C., Incagli, M., Jia, Yi, Jinchi, H., Kanishev, K., Khiali, B., Kirn, Th., Konak, C., Kounina, O., Kounine, A., Koutsenko, V., Kulemzin, A., La Vacca, G., Laudi, E., Laurenti, G., Lazzizzera, I., Lebedev, A., Lee, H.T., Lee, S.C., Leluc, C., Li, J.Q., Li, Q., Li, T.X., Li, Z.H., Light, C., Lin, C.H., Lippert, T., Liu, F.Z., Liu, Hu, Liu, Z., Lu, S.Q., Lu, Y.S., Luebelsmeyer, K., Luo, F., Luo, J.Z., Luo, Xi, Lyu, S.S., MacHate, F., Mañá, C., Marín, J., Martin, T., Martínez, G., Masi, N., Maurin, D., Menchaca-Rocha, A., Meng, Q., Mo, D.C., Molero, M., Mott, P., Mussolin, L., Nelson, T., Ni, J.Q., Nikonov, N., Nozzoli, F., Oliva, A., Orcinha, M., Palermo, M., Palmonari, F., Paniccia, M., Pashnin, A., Pauluzzi, M., Pensotti, S., Perrina, C., Phan, H.D., Picot-Clemente, N., Plyaskin, V., Pohl, M., Poireau, V., Popkow, A., Quadrani, L., Qi, X.M., Qin, X., Qu, Z.Y., Rancoita, P.G., Rapin, D., Conde, A. Reina, Rosier-Lees, S., Rozhkov, A., Rozza, D., Sagdeev, R., Solano, C., Schael, S., Schmidt, S.M., Schulz Von Dratzig, A., Schwering, G., Seo, E.S., Shan, B.S., Shi, J.Y., Siedenburg, T., Song, J.W., Sun, Z.T., Tacconi, M., Tang, X.W., Tang, Z.C., Tian, J., Ting, Samuel C. C., Ting, S.M., Tomassetti, N., Torsti, J., Urban, T., Vagelli, V., Valente, E., Valtonen, E., Vázquez Acosta, M., Vecchi, M., Velasco, M., Vialle, J.P., Vizán, J., Wang, L.Q., Wang, N.H., Wang, Q.L., Wang, X., Wang, X.Q., Wang, Z.X., Wei, J., Weng, Z.L., Wu, H., Xiong, R.Q., Xu, W., Yan, Q., Yang, Y., Yi, H., Yu, Y.J., Yu, Z.Q., Zannoni, M., Zeissler, S., Zhang, C., Zhang, F., Zhang, J.H., Zhang, Z., Zhao, F., Zheng, Z.M., Zhuang, H.L., Zhukov, V., Zichichi, A., Zimmermann, N., Zuccon, P., Research unit Astroparticle Physics, Azzarello, Philipp, Bourquin, Maurice, Chen, Yao, Leluc, Catherine, Liu, Zhen, Paniccia, Mercedes, Perrina, Chiara, Pohl, Martin, Rapin, Divic Jean, Wei, Jiahui, Massachusetts Institute of Technology. Department of Physics, Massachusetts Institute of Technology. Laboratory for Nuclear Science, Becker, Ulrich J, Behlmann, Matthew Daniel, Burger, Joseph D, Cai, Xudong, Capell, Michael H, Choutko, Vitali, Egorov, Alexander, Eline, Alexandre, Fisher, Peter H, Heil, Melanie, Hsieh, Timothy Hwa-wei, Kounina, Olga, Kounine, Andrei, Koutsenko, Vladimir, Kulemzin, Alexander, Lebedev, Alexei, Liu, F. Z., Phan, Huy Duc, Plyaskin, Vasily, Qin, Xiaoting, Ting, Samuel, Ting, Steve M, Yan, Qi, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), and Laboratoire d'Annecy de Physique des Particules (LAPP)
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General Physics and Astronomy ,Flux ,Electron ,positron: flux ,Astrophysics ,01 natural sciences ,Spectral line ,Space detectors ,Positron ,Alpha Magnetic Spectrometer ,Dark Matter ,Cutoff ,AMS ,010303 astronomy & astrophysics ,energy: low ,Physics ,Range (particle radiation) ,energy: high ,Spectrometers ,AMS02 ,Complex energy ,Cosmology ,FIS/01 - FISICA SPERIMENTALE ,Atomic physics ,Particle astrophysics ,Cosmic ray composition, spectraCosmic ray propagation, Cosmic ray sources, Particle astrophysics, Particle dark matter, Gravitation, Cosmology, Astrophysics ,positron: cosmic radiation ,Gravitation ,spectraCosmic ray propagation ,Astrophysics and Astronomy ,Astrophysics::High Energy Astrophysical Phenomena ,satellite ,Cosmic ray ,ddc:500.2 ,International Space stations ,Gravitation and Astrophysics ,energy dependence ,Physics and Astronomy (all) ,FIS/05 - ASTRONOMIA E ASTROFISICA ,Particle dark matter ,Cosmic ray composition ,Cosmic-ray positrons ,0103 physical sciences ,Dark matter ,ddc:530 ,Cosmic Rays, positrons ,finite energy ,Cosmic rays ,ta115 ,010308 nuclear & particles physics ,dark matter: annihilation ,Cosmic ray sources ,ASTROFÍSICA ,magnetic spectrometer ,Physics::Accelerator Physics ,High Energy Physics::Experiment ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] - Abstract
Physical review letters 122(4), 041102 (2019). doi:10.1103/PhysRevLett.122.041102, Published by APS, College Park, Md.
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- 2019
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13. First Analysis of Ground-Level Enhancement (GLE) 72 on 10 September 2017: Spectral and Anisotropy Characteristics
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Rami Vainio, Miikka Paassilta, Ilya Usoskin, Alexander Mishev, Eino Valtonen, Leon Kocharov, and Osku Raukunen
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Physics ,010504 meteorology & atmospheric sciences ,Basis (linear algebra) ,Magnetosphere ,Astronomy and Astrophysics ,Rigidity (psychology) ,Solar cycle 24 ,01 natural sciences ,Spectral line ,Computational physics ,Space and Planetary Science ,0103 physical sciences ,Neutron ,Anisotropy ,010303 astronomy & astrophysics ,Event (particle physics) ,0105 earth and related environmental sciences - Abstract
Using data obtained with neutron monitors and space-borne instruments, we analyzed the second ground-level enhancement (GLE) of Solar Cycle 24, namely the event of 10 September 2017 (GLE 72), and derived the spectral and angular characteristics of associated GLE particles. We employed a new neutron-monitor yield function and a recently proposed model based on an optimization procedure. The method consists of simulating particle propagation in a model magnetosphere in order to derive the cutoff rigidity and neutron-monitor asymptotic directions. Subsequently, the rigidity spectrum and anisotropy of GLE particles are obtained in their dynamical evolution during the event on the basis of an inverse-problem solution. The derived angular distribution and spectra are discussed briefly.
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- 2018
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14. Interplanetary fast forward shocks and energetic storm particle events above 1.5 MeV
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Eino Valtonen and K. Huttunen-Heikinmaa
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Atmospheric Science ,010504 meteorology & atmospheric sciences ,Astrophysics ,01 natural sciences ,Power law ,Standard deviation ,Relativistic particle ,0103 physical sciences ,Earth and Planetary Sciences (miscellaneous) ,lcsh:Science ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences ,Physics ,Spectral index ,Shock (fluid dynamics) ,lcsh:QC801-809 ,Geology ,Astronomy and Astrophysics ,Solar physics ,lcsh:QC1-999 ,Solar cycle ,lcsh:Geophysics. Cosmic physics ,13. Climate action ,Space and Planetary Science ,lcsh:Q ,Interplanetary spaceflight ,lcsh:Physics - Abstract
Interplanetary (IP) shock passages are usually identified by abrupt changes in the plasma parameters, but sometimes they are also associated with energetic storm particles (ESPs). The maximum observed energies of ESPs usually reach a few MeVs per nucleon and occasionally even a few hundred MeVs per nucleon. We have carried out a statistical study of ESP events observed by SOHO/ERNE above 1.5 MeV during the seven-year period between May 1996 and April 2003. In the first stage, we gathered a comprehensive database of IP shock candidates using several ready-made shock lists. We defined a qualitative classification for the ESP signals and studied their association with fast forward shocks. We present a survey of the overall statistics of ESP associations with fast forward shocks and the yearly amount of the shocks and associated ESP events during the 7-year study period. Our most important findings are that only 40% of the observed interplanetary fast forward shocks accelerate ESPs to energies greater than 1.5 MeV and that the high-energy ESP-effectiveness of the fast forward shocks has a solar cycle dependence. The yearly ESP-effectiveness varied from 11%, in May 1996–April 1997 (~activity minimum), to 53% in May 2000–April 2001 (~activity maximum). We also performed a quantitative analysis of the proton power law spectra at the time of the shock passage. We found that the average spectral index of ESPs was −3.6 with the standard deviation of the distribution of 1.3. The ESP events had significantly larger power law factors than the reference spectra, calculated every day at a certain time for comparison.
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- 2018
15. Precision Measurement of Cosmic-Ray Nitrogen and its Primary and Secondary Components with the Alpha Magnetic Spectrometer on the International Space Station
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Giovanni Ambrosi, Yu. Galaktionov, K. F. Bindel, H. T. Lee, J. Q. Ni, A. Egorov, F. Dimiccoli, Carlos Díaz, W. De Boer, C. Clark, M. Graziani, O. Kounina, H. Wu, Andrea Contin, G. Coignet, A. Ghelfi, Valery Zhukov, J. D. Burger, T. Siedenburg, Claudio Corti, V. Poireau, C. Konak, F. Palmonari, R. J. García-López, A. Datta, K. Whitman, W. J. Burger, D. Rozza, V. D. Lordello, A. I. Chen, Jonathan L. Feng, S. Başeğmez-du Pree, T. J. N. Nelson, D. C. Mo, Shihao Zhang, V Vagelli, Hui Li, Z. Q. Yu, F. Dong, S. Caroff, P. von Doetinchem, X. D. Cai, J. J. Torsti, S. Pensotti, Antonino Zichichi, S. M. Ting, H. Yi, M. Pauluzzi, L Mussolin, F. Cervelli, N. Attig, S. Di Falco, D. M. Gómez-Coral, G. La Vacca, David Maurin, F. Donnini, Manuela Vecchi, W. Creus, K. H. Guo, A. Lebedev, Corinne Goy, Roald Z. Sagdeev, S. Della Torre, S. Rosier-Lees, M. Crispoltoni, V. M. Mikuni, G. Schwering, Laurent Derome, M. Pohl, M. Aguilar, C. Consolandi, L. Ali Cavasonza, J. Z. Luo, Lucio Quadrani, Y. Chen, Z Liu, Mario Zannoni, Z. L. Weng, H. P. Huang, D. Rapin, V. Plyaskin, I. Lazzizzera, H. Jinchi, Samuel C.C. Ting, Yuan-Hann Chang, A. Bachlechner, E. Valente, M. Incagli, Liqiu Wang, P. Mott, C. Mañá, Mauro Tacconi, Veronica Bindi, P. Lipari, Yang Yang, B. S. Shan, T. Räihä, M. B. Demirköz, Roberto Battiston, Chuanguo Zhang, T. Martin, J Wei, D. Grandi, K. Dadzie, Nicola Tomassetti, Henning Gast, Eun-Suk Seo, X. Q. Wang, Ying Lu, T. Kirn, T. Urban, V. Choutko, B. Borgia, Lin Cheng, B. Bertucci, M. Paniccia, E. Choumilov, Paolo Zuccon, Behcet Alpat, H. D. Phan, F. Barao, A. Rozhkov, K. C. Han, X. W. Tang, Massimo Gervasi, Q. L. Wang, V. Koutsenko, Eino Valtonen, R. Clavero, N. Picot-Clemente, Matteo Boschini, Timothy H. Hsieh, Y. J. Yu, F. Giovacchini, U. Becker, Yi Jia, C. Perrina, C. Delgado, J. P. Vialle, B. Khiali, L. Basara, M. Orcinha, Thomas Lippert, Hu Liu, Zhixiang Tang, T. X. Li, Varlen Grabski, Zhihua Zhang, M. Bourquin, J. Zhang, N. Masi, F. Luo, L. Barrin, A. Schulz von Dratzig, D. Tescaro, P. H. Fisher, Andrei Kounine, J. Q. Li, S. Aupetit, Z. M. Zheng, Q. Yan, M. Capell, D. Liu, G. Martinez, C. Palomares, E. F. Bueno, Xiaoqun Wang, J Tian, Z. H. Li, Qiang Li, A. Barrau, A. Kulemzin, N. Zimmermann, Zhao Wang, Luísa Arruda, F. Machate, G. Castellini, R. Q. Xiong, S. Zeissler, Z. Y. Qu, H. Y. Chou, Mayda Velasco, Q. Meng, I. Gebauer, S. M. Schmidt, J. Berdugo, Z. Cui, X. Qin, Sadakazu Haino, Fabrizio Giulio Luca Pilo, M. Vazquez Acosta, A. Eline, K. Bollweg, Naihua Wang, K. Luebelsmeyer, Guo-Ming Chen, Chia-Hui Lin, J. Gong, J. Y. Shi, N. Nikonov, Julio C. Marín, E. Fiandrini, J. W. Song, M. Duranti, H. S. Chen, J. Casaus, C. C. Wei, Z. Y. Li, P. G. Rancoita, Mingming Yang, Valerio Formato, S. Schael, Elisa Laudi, Arturo Alejandro Menchaca-Rocha, Markus Battarbee, J. H. Zhang, Corrado Gargiulo, Z. H. He, F. Nozzoli, T. Eronen, P. Azzarello, W. Xu, Zhiqi Huang, S. C. Lee, X. M. Qi, C. H. Chung, J. S. Ricol, M. Behlmann, Matthias Heil, G. Laurenti, M. Palermo, K. Kanishev, A. Bartoloni, Fan Zhang, S. S. Lyu, A. Oliva, C. Leluc, G. Gallucci, Yaomin Dai, S. Q. Lu, H. L. Zhuang, B. Beischer, V. Bonnivard, Research unit Astroparticle Physics, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), 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), AMS, Aguilar, M., Ali Cavasonza, L., Alpat, B., Ambrosi, G., Arruda, L., Attig, N., Aupetit, S., Azzarello, P., Bachlechner, A., Barao, F., Barrau, A., Barrin, L., Bartoloni, A., Basara, L., Başeǧmez-Du Pree, S., Battarbee, M., Battiston, R., Becker, U., Behlmann, M., Beischer, B., Berdugo, J., Bertucci, B., Bindel, K.F., Bindi, V., De Boer, W., Bollweg, K., Bonnivard, V., Borgia, B., Boschini, M.J., Bourquin, M., Bueno, E.F., Burger, J., Burger, W.J., Cai, X.D., Capell, M., Caroff, S., Casaus, J., Castellini, G., Cervelli, F., Chang, Y.H., Chen, A.I., Chen, G.M., Chen, H.S., Chen, Y., Cheng, L., Chou, H.Y., Choumilov, E., Choutko, V., Chung, C.H., Clark, C., Clavero, R., Coignet, G., Consolandi, C., Contin, A., Corti, C., Creus, W., Crispoltoni, M., Cui, Z., Dadzie, K., Dai, Y.M., Datta, A., Delgado, C., Della Torre, S., Demirköz, M.B., Derome, L., Di Falco, S., Dimiccoli, F., Díaz, C., Von Doetinchem, P., Dong, F., Donnini, F., Duranti, M., Egorov, A., Eline, A., Eronen, T., Feng, J., Fiandrini, E., Fisher, P., Formato, V., Galaktionov, Y., Gallucci, G., García-López, R.J., Gargiulo, C., Gast, H., Gebauer, I., Gervasi, M., Ghelfi, A., Giovacchini, F., Gómez-Coral, D.M., Gong, J., Goy, C., Grabski, V., Grandi, D., Graziani, M., Guo, K.H., Haino, S., Han, K.C., He, Z.H., Heil, M., Hsieh, T.H., Huang, H., Huang, Z.C., Incagli, M., Jia, Yi, Jinchi, H., Kanishev, K., Khiali, B., Kirn, Th., Konak, C., Kounina, O., Kounine, A., Koutsenko, V., Kulemzin, A., La Vacca, G., Laudi, E., Laurenti, G., Lazzizzera, I., Lebedev, A., Lee, H.T., Lee, S.C., Leluc, C., Li, H.S., Li, J.Q., Li, Q., Li, T.X., Li, Z.H., Li, Z.Y., Lin, C.H., Lipari, P., Lippert, T., Liu, D., Liu, Hu, Liu, Z., Lordello, V.D., Lu, S.Q., Lu, Y.S., Luebelsmeyer, K., Luo, F., Luo, J.Z., Lyu, S.S., Machate, F., Mañá, C., Marín, J., Martin, T., Martínez, G., Masi, N., Maurin, D., Menchaca-Rocha, A., Meng, Q., Mikuni, V.M., Mo, D.C., Mott, P., Mussolin, L., Nelson, T., Ni, J.Q., Nikonov, N., Nozzoli, F., Oliva, A., Orcinha, M., Palermo, M., Palmonari, F., Palomares, C., Paniccia, M., Pauluzzi, M., Pensotti, S., Perrina, C., Phan, H.D., Picot-Clemente, N., Pilo, F., Plyaskin, V., Pohl, M., Poireau, V., Quadrani, L., Qi, X.M., Qin, X., Qu, Z.Y., Räihä, T., Rancoita, P.G., Rapin, D., Ricol, J.S., Rosier-Lees, S., Rozhkov, A., Rozza, D., Sagdeev, R., Schael, S., Schmidt, S.M., Schulz Von Dratzig, A., Schwering, G., Seo, E.S., Shan, B.S., Shi, J.Y., Siedenburg, T., Song, J.W., Tacconi, M., Tang, X.W., Tang, Z.C., Tescaro, D., Tian, J., Ting, Samuel C. C., Ting, S.M., Tomassetti, N., Torsti, J., Urban, T., Vagelli, V., Valente, E., Valtonen, E., Vázquez Acosta, M., Vecchi, M., Velasco, M., Vialle, J.P., Wang, L.Q., Wang, N.H., Wang, Q.L., Wang, X., Wang, X.Q., Wang, Z.X., Wei, C.C., Wei, J., Weng, Z.L., Whitman, K., Wu, H., Xiong, R.Q., Xu, W., Yan, Q., Yang, M., Yang, Y., Yi, H., Yu, Y.J., Yu, Z.Q., Zannoni, M., Zeissler, S., Zhang, C., Zhang, F., Zhang, J., Zhang, J.H., Zhang, S.W., Zhang, Z., Zheng, Z.M., Zhuang, H.L., Zhukov, V., Zichichi, A., Zimmermann, N., Zuccon, P., Azzarello, Philipp, Bourquin, Maurice, Chen, Yao, Leluc, Catherine, Liu, Zhen, Paniccia, Mercedes, Perrina, Chiara, Pohl, Martin, Rapin, Divic Jean, Wei, Jiahui, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Laboratoire d'Annecy de Physique des Particules (LAPP), Massachusetts Institute of Technology. Department of Nuclear Science and Engineering, Massachusetts Institute of Technology. Department of Physics, Massachusetts Institute of Technology. Laboratory for Nuclear Science, Becker, Ulrich J, Behlmann, Matthew Daniel, Burger, Joseph D, Cai, Xudong, Capell, Michael H, Chen, Andrew I, Choumilov, Evgueni, Choutko, Vitali, Egorov, Alexander, Eline, Alexandre, Feng, Jie, Fisher, Peter H, Heil, Melanie, Hsieh, Timothy Hwa-wei, Kounina, Olga, Kounine, Andrei, Koutsenko, Vladimir, Kulemzin, Alexander, Lebedev, Alexei, Phan, Huy Duc, Plyaskin, Vasily, Qin, Xiaoting, Rozhkov, Andrey B., Ting, Samuel, Yan, Qi, Zhang, Jing, Zhang, Zhan, Zuccon, Paolo, Aguilar, M, Ali Cavasonza, L, Alpat, B, Ambrosi, G, Arruda, L, Attig, N, Aupetit, S, Azzarello, P, Bachlechner, A, Barao, F, Barrau, A, Barrin, L, Bartoloni, A, Basara, L, Başeğmez-du Pree, S, Battarbee, M, Battiston, R, Becker, U, Behlmann, M, Beischer, B, Berdugo, J, Bertucci, B, Bindel, K, Bindi, V, de Boer, W, Bollweg, K, Bonnivard, V, Borgia, B, Boschini, M, Bourquin, M, Bueno, E, Burger, J, Burger, W, Cai, X, Capell, M, Caroff, S, Casaus, J, Castellini, G, Cervelli, F, Chang, Y, Chen, A, Chen, G, Chen, H, Chen, Y, Cheng, L, Chou, H, Choumilov, E, Choutko, V, Chung, C, Clark, C, Clavero, R, Coignet, G, Consolandi, C, Contin, A, Corti, C, Creus, W, Crispoltoni, M, Cui, Z, Dadzie, K, Dai, Y, Datta, A, Delgado, C, Della Torre, S, Demirköz, M, Derome, L, Di Falco, S, Dimiccoli, F, Díaz, C, von Doetinchem, P, Dong, F, Donnini, F, Duranti, M, Egorov, A, Eline, A, Eronen, T, Feng, J, Fiandrini, E, Fisher, P, Formato, V, Galaktionov, Y, Gallucci, G, García-López, R, Gargiulo, C, Gast, H, Gebauer, I, Gervasi, M, Ghelfi, A, Giovacchini, F, Gómez-Coral, D, Gong, J, Goy, C, Grabski, V, Grandi, D, Graziani, M, Guo, K, Haino, S, Han, K, He, Z, Heil, M, Hsieh, T, Huang, H, Huang, Z, Incagli, M, Jia, Y, Jinchi, H, Kanishev, K, Khiali, B, Kirn, T, Konak, C, Kounina, O, Kounine, A, Koutsenko, V, Kulemzin, A, La Vacca, G, Laudi, E, Laurenti, G, Lazzizzera, I, Lebedev, A, Lee, H, Lee, S, Leluc, C, Li, H, Li, J, Li, Q, Li, T, Li, Z, Lin, C, Lipari, P, Lippert, T, Liu, D, Liu, H, Liu, Z, Lordello, V, Lu, S, Lu, Y, Luebelsmeyer, K, Luo, F, Luo, J, Lyu, S, Machate, F, Mañá, C, Marín, J, Martin, T, Martínez, G, Masi, N, Maurin, D, Menchaca-Rocha, A, Meng, Q, Mikuni, V, Mo, D, Mott, P, Mussolin, L, Nelson, T, Ni, J, Nikonov, N, Nozzoli, F, Oliva, A, Orcinha, M, Palermo, M, Palmonari, F, Palomares, C, Paniccia, M, Pauluzzi, M, Pensotti, S, Perrina, C, Phan, H, Picot-Clemente, N, Pilo, F, Plyaskin, V, Pohl, M, Poireau, V, Quadrani, L, Qi, X, Qin, X, Qu, Z, Räihä, T, Rancoita, P, Rapin, D, Ricol, J, Rosier-Lees, S, Rozhkov, A, Rozza, D, Sagdeev, R, Schael, S, Schmidt, S, Schulz von Dratzig, A, Schwering, G, Seo, E, Shan, B, Shi, J, Siedenburg, T, Song, J, Tacconi, M, Tang, X, Tang, Z, Tescaro, D, Tian, J, Ting, S, Tomassetti, N, Torsti, J, Urban, T, Vagelli, V, Valente, E, Valtonen, E, Vázquez Acosta, M, Vecchi, M, Velasco, M, Vialle, J, Wang, L, Wang, N, Wang, Q, Wang, X, Wang, Z, Wei, C, Wei, J, Weng, Z, Whitman, K, Wu, H, Xiong, R, Xu, W, Yan, Q, Yang, M, Yang, Y, Yi, H, Yu, Y, Yu, Z, Zannoni, M, Zeissler, S, Zhang, C, Zhang, F, Zhang, J, Zhang, S, Zhang, Z, Zheng, Z, Zhuang, H, Zhukov, V, Zichichi, A, Zimmermann, N, and Zuccon, P
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General Physics and Astronomy ,power spectrum ,Galactic cosmic rays ,01 natural sciences ,nitrogen ,CARBON ,ddc:550 ,Alpha Magnetic Spectrometer ,Primary component ,AMS ,010303 astronomy & astrophysics ,Physics ,Spectral index ,FLIGHT ,Spectrometers ,precision measurement ,AMS02 ,Nitrogen ,FIS/01 - FISICA SPERIMENTALE ,CHARGE COMPOSITION ,Astrophysics and Astronomy ,Astrophysics::High Energy Astrophysical Phenomena ,satellite ,chemistry.chemical_element ,Cosmic ray ,ddc:500.2 ,helium ,Astrophysics::Cosmology and Extragalactic Astrophysics ,International Space stations ,Cosmic Rays, Antimatter, Alpha Magnetic Spectrometer, International Space Station ,Nuclear physics ,FIS/05 - ASTRONOMIA E ASTROFISICA ,Physics and Astronomy (all) ,ABUNDANCES ,Secondary cosmic-rays ,AMS-02 ,0103 physical sciences ,ENERGY-SPECTRA ,ddc:530 ,boron: flux ,010306 general physics ,cosmic radiation: secondary ,DETECTOR ,Helium ,ta115 ,NUCLEI ,Primary comsic-rays ,Cosmic-ray nitrogen ,Unit charge ,Spectral density ,COSMIC RAYS ,ASTROFÍSICA ,Optical waveguides ,cosmic radiation: primary ,chemistry ,spectral ,GEOMAGNETIC REFERENCE FIELD ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,oxygen ,GENERATION - Abstract
Physical review letters 121(5), 051103 (2018). doi:10.1103/PhysRevLett.121.051103, Published by APS, College Park, Md.
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- 2018
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16. Nowcasting Solar Energetic Particle Events Using Principal Component Analysis
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Maria Abunina, Anastasios Anastasiadis, A. A. Abunin, Eino Valtonen, Athanasios Papaioannou, Rami Vainio, E. A. Eroshenko, Miikka Paassilta, A. Kouloumvakos, and A. V. Belov
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Physics ,010504 meteorology & atmospheric sciences ,Logarithm ,Solar flare ,Order (ring theory) ,Astronomy and Astrophysics ,01 natural sciences ,Base (group theory) ,Space and Planetary Science ,0103 physical sciences ,Principal component analysis ,Coronal mass ejection ,Statistical physics ,010303 astronomy & astrophysics ,Categorical variable ,0105 earth and related environmental sciences ,Event (probability theory) - Abstract
We perform a principal component analysis (PCA) on a set of six solar variables (i.e. width/size ( $s$ ) and velocity ( $u$ ) of a coronal mass ejection, logarithm of the solar flare (SF) magnitude ( $\log\mathit{SXRs}$ ), SF longitude ( $\mathit{lon}$ ), duration ( $\mathit{DT}$ ), and rise time ( $\mathit{RT}$ )). We classify the solar energetic particle (SEP) event radiation impact (in terms of the National Oceanic and Atmospheric Administration scales) with respect to the characteristics of their parent solar events. We further attempt to infer the possible prediction of SEP events. In our analysis, we use 126 SEP events with complete solar information, from 1997 to 2013. Each SEP event is a vector in six dimensions (corresponding to the six solar variables used in this work). The PCA transforms the input vectors into a set of orthogonal components. By mapping the characteristics of the parent solar events, a new base defined by these components led to the classification of the SEP events. We furthermore applied logistic regression analysis with single, as well as multiple explanatory variables, in order to develop a new index ( $I$ ) for the nowcasting (short-term forecasting) of SEP events. We tested several different schemes for $I$ and validated our findings with the implementation of categorical scores (probability of detection (POD) and false-alarm rate (FAR)). We present and interpret the obtained scores, and discuss the strengths and weaknesses of the different implementations. We show that $I$ holds prognosis potential for SEP events. The maximum POD achieved is 77.78% and the relative FAR is 40.96%.
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- 2018
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17. Catalogue of > 55 ${>}\,55$ MeV Wide-longitude Solar Proton Events Observed by SOHO, ACE, and the STEREOs at ≈ 1 ${\approx}\,1$ AU During 2009 – 2016
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Rami Vainio, Nina Dresing, Eino Valtonen, Bernd Heber, Miikka Paassilta, and Athanasios Papaioannou
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Physics ,Solar phenomena ,010504 meteorology & atmospheric sciences ,Proton ,Astronomy and Astrophysics ,Astrophysics ,Electron ,Kinetic energy ,7. Clean energy ,01 natural sciences ,law.invention ,Particle acceleration ,13. Climate action ,Space and Planetary Science ,law ,Physics::Space Physics ,0103 physical sciences ,Coronal mass ejection ,Astrophysics::Solar and Stellar Astrophysics ,Large Angle and Spectrometric Coronagraph ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences ,Flare - Abstract
Based on energetic particle observations made at ${\approx}\,1$ AU, we present a catalogue of 46 wide-longitude ( ${>}\,45^{\circ}$ ) solar energetic particle (SEP) events detected at multiple locations during 2009 – 2016. The particle kinetic energies of interest were chosen as ${>}\,55$ MeV for protons and 0.18 – 0.31 MeV for electrons. We make use of proton data from the Solar and Heliospheric Observatory/Energetic and Relativistic Nuclei and Electron Experiment (SOHO/ERNE) and the Solar Terrestrial Relations Observatory/High Energy Telescopes (STEREO/HET), together with electron data from the Advanced Composition Explorer/Electron, Proton, and Alpha Monitor (ACE/EPAM) and the STEREO/Solar Electron and Proton Telescopes (SEPT). We consider soft X-ray data from the Geostationary Operational Environmental Satellites (GOES) and coronal mass ejection (CME) observations made with the SOHO/Large Angle and Spectrometric Coronagraph (LASCO) and STEREO/Coronagraphs 1 and 2 (COR1, COR2) to establish the probable associations between SEP events and the related solar phenomena. Event onset times and peak intensities are determined; velocity dispersion analysis (VDA) and time-shifting analysis (TSA) are performed for protons; TSA is performed for electrons. In our event sample, there is a tendency for the highest peak intensities to occur when the observer is magnetically connected to solar regions west of the flare. Our estimates for the mean event width, derived as the standard deviation of a Gaussian curve modelling the SEP intensities (protons ${\approx}\,44^{\circ}$ , electrons ${\approx}\,50^{\circ}$ ), largely agree with previous results for lower-energy SEPs. SEP release times with respect to event flares, as well as the event rise times, show no simple dependence on the observer’s connection angle, suggesting that the source region extent and dominant particle acceleration and transport mechanisms are important in defining these characteristics of an event. There is no marked difference between the speed distributions of the CMEs related to wide events and the CMEs related to all near-Earth SEP events of similar energy range from the same time period.
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- 2018
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18. Fabrication of a thin silicon detector with excellent thickness uniformity
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T. Eronen, Hannu Husu, K. Miikkulainen, Eino Valtonen, M. Hirvonen, Hans Andersson, J. Mäkinen, S. Nenonen, Hannu Ronkainen, Simo Eränen, Risto Punkkinen, and Antti Lassila
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Solar energetic particles ,ΔE-E ,Nuclear and High Energy Physics ,Fizeau interferometer ,Silicon detector ,Fabrication ,Silicon ,Physics::Instrumentation and Detectors ,chemistry.chemical_element ,Silicon on insulator ,01 natural sciences ,law.invention ,Telescope ,[omega]E-E ,Optics ,law ,0103 physical sciences ,010303 astronomy & astrophysics ,Instrumentation ,ta212 ,Physics ,ta115 ,ta213 ,ta114 ,010308 nuclear & particles physics ,business.industry ,Detector ,SOI technology ,Thickness uniformity ,chemistry ,High Energy Physics::Experiment ,business - Abstract
We have fabricated and tested a thin silicon detector with the specific goal of having a very good thickness uniformity. SOI technology was used in the detector fabrication. The detector was designed to be used as a ΔE detector in a silicon telescope for measuring solar energetic particles in space. The detector thickness was specified to be 20 μm with an rms thickness uniformity of±0.5%. The active area consists of three separate elements, a round centre area and two surrounding annular segments. A new method was developed for measuring the thickness uniformity based on a modified Fizeau interferometer. The thickness uniformity specification was well met with the measured rms thickness variation of 43 nm. The detector was electrically characterized by measuring the I – V and C – V curves and the performance was verified using a 241Am alpha source.
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- 2016
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19. Formation of Radio Type II Bursts During a Multiple Coronal Mass Ejection Event
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Silja Pohjolainen, Eino Valtonen, and Firas Al-Hamadani
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Physics ,Wavelength ,010504 meteorology & atmospheric sciences ,Density gradient ,Space and Planetary Science ,0103 physical sciences ,Coronal mass ejection ,Astronomy and Astrophysics ,Astrophysics ,Wake ,010303 astronomy & astrophysics ,01 natural sciences ,0105 earth and related environmental sciences - Abstract
We study the solar event on 27 September 2001 that consisted of three consecutive coronal mass ejections (CMEs) originating from the same active region, which were associated with several periods of radio type II burst emission at decameter–hectometer (DH) wavelengths. Our analysis shows that the first radio burst originated from a low-density environment, formed in the wake of the first, slow CME. The frequency-drift of the burst suggests a low-speed burst driver, or that the shock was not propagating along the large density gradient. There is also evidence of band-splitting within this emission lane. The origin of the first shock remains unclear, as several alternative scenarios exist. The second shock showed separate periods of enhanced radio emission. This shock could have originated from a CME bow shock, caused by the fast and accelerating second or third CME. However, a shock at CME flanks is also possible, as the density depletion caused by the three CMEs would have affected the emission frequencies and hence the radio source heights could have been lower than usual. The last type II burst period showed enhanced emission in a wider bandwidth, which was most probably due to the CME–CME interaction. Only one shock that could reliably be associated with the investigated CMEs was observed to arrive near Earth.
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- 2017
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20. Origin of Radio Enhancements in Type II Bursts in the Outer Corona
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Firas Al-Hamadani, Silja Pohjolainen, and Eino Valtonen
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Physics ,010504 meteorology & atmospheric sciences ,Shock (fluid dynamics) ,Front (oceanography) ,Astronomy ,Astronomy and Astrophysics ,Astrophysics ,Electron ,Solar radio ,01 natural sciences ,Corona ,law.invention ,Space and Planetary Science ,law ,0103 physical sciences ,Coronal mass ejection ,Interplanetary spaceflight ,010303 astronomy & astrophysics ,Coronagraph ,0105 earth and related environmental sciences - Abstract
We study interplanetary (IP) solar radio type II bursts from 2011 – 2014 in order to determine the cause of the intense enhancements in their radio emission. Type II bursts are known to be due to propagating shocks that are often associated with fast halo-type coronal mass ejections (CMEs). We analysed the radio spectral data and the white-light coronagraph data from 16 selected events to obtain directions and heights for the propagating CMEs and the type II bursts. CMEs preceding the selected events were included in the analysis to verify whether CME interaction was possible. As a result, we were able to classify the events into five different groups. 1) Events where the heights of the CMEs and type II bursts are consistent, indicating that the shock is located at the leading front of the CME. The radio enhancements are superposed on the type II lanes, and they are probably formed when the shock meets remnant material from earlier CMEs, but the shock continues to propagate at the same speed. 2) Events where the type II heights agree with the CME leading front and an earlier CME is located at a height that suggests interaction. The radio enhancements and frequency jumps could be due to the merging process of the CMEs. 3) Events where the type II heights are significantly lower than the CME heights almost from the start. Interaction with close-by streamers is probably the cause for the enhanced radio emission, which is located at the CME flank region. 4) Events where the radio enhancements are located within wide-band type II bursts and the causes for the radio enhancements are not clear. 5) Events where the radio enhancements are associated with later-accelerated particles (electron beams, observed as type III bursts) that stop at the type II burst emission lane, and no other obvious reason for the enhancement can be identified. Most of the events (38%) were due to shock–streamer interaction, while one quarter of the events was due to possible CME–CME interaction. The drift rates, bandwidth characteristics, or cross-correlations of various characteristics did not reveal any clear association with particular category types. The chosen atmospheric density model causes the largest uncertainties in the derived radio heights, although in some cases, the emission bandwidths also lead to relatively large error margins. Our conclusion is that the enhanced radio emission associated with CMEs and propagating shocks can have different origins, depending on their overall configuration and the associated processes.
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- 2017
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21. X-Ray, Radio and SEP Observations of Relativistic Gamma-Ray Events
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Jurgen Kiener, Bernd Heber, C. Hamadache, Nicole Vilmer, Karl-Ludwig Klein, Pietro Zucca, Olga Malandraki, Kostas Tziotziou, and Eino Valtonen
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Physics ,Photon ,010504 meteorology & atmospheric sciences ,Solar energetic particles ,Astrophysics::High Energy Astrophysical Phenomena ,X-ray ,Gamma ray ,Phase (waves) ,Astrophysics ,01 natural sciences ,Particle acceleration ,Electron acceleration ,0103 physical sciences ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences ,Fermi Gamma-ray Space Telescope - Abstract
The rather frequent occurrence, and sometimes long duration, of γ-ray events at photon energies above 100 MeV challenges our understanding of particle acceleration processes at the Sun. The emission is ascribed to pion-decay photons due to protons with energies above 300 MeV. We study the X-ray and radio emissions and the solar energetic particles (SEPs) in space for a set of 25 Fermi γ-ray events. They are accompanied by strong SEP events, including, in most cases where the parent activity is well-connected, protons above 300 MeV. Signatures of energetic electron acceleration in the corona accompany the impulsive and early post-impulsive γ-ray emission. γ-ray emission lasting several hours accompanies in general the decay phase of long-lasting soft X-ray bursts and decametric-to-kilometric type II bursts. We discuss the impact of these results on the origin of the γ-ray events.
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- 2017
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22. Investigation of the Geoeffectiveness of Disk-Centre Full-Halo Coronal Mass Ejections
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Eino Valtonen and Dheyaa Ameri
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Geomagnetic storm ,Physics ,010504 meteorology & atmospheric sciences ,Solar cycle 23 ,Astronomy ,Magnetosphere ,Flux ,Astronomy and Astrophysics ,01 natural sciences ,Solar wind ,Space and Planetary Science ,0103 physical sciences ,Coronal mass ejection ,Interplanetary magnetic field ,Interplanetary spaceflight ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences - Abstract
We studied the occurrence and characteristics of geomagnetic storms associated with disk-centre full-halo coronal mass ejections (DC-FH-CMEs). Such coronal mass ejections (CMEs) can be considered as the most plausible cause of geomagnetic storms. We selected front-side full-halo coronal mass ejections detected by the Large Angle and Spectrometric Coronagraph onboard the Solar and Heliospheric Observatory (SOHO/LASCO) from the beginning of 1996 till the end of 2015 with source locations between solar longitudes E10 and W10 and latitudes N20 and S20. The number of selected CMEs was 66 of which 33 (50%) were deduced to be the cause of 30 geomagnetic storms with $\mathrm{Dst} \leq- 50~\mbox{nT}$ . Of the 30 geomagnetic storms, 26 were associated with single disk-centre full-halo CMEs, while four storms were associated, in addition to at least one disk-centre full-halo CME, also with other halo or wide CMEs from the same active region. Thirteen of the 66 CMEs (20%) were associated with 13 storms with $-100~\mbox{nT} < \mbox{Dst} \leq- 50~\mbox{nT}$ , and 20 (30%) were associated with 17 storms with $\mbox{Dst}\leq- 100~\mbox{nT}$ . We investigated the distributions and average values of parameters describing the DC-FH-CMEs and their interplanetary counterparts encountering Earth. These parameters included the CME sky-plane speed and direction parameter, associated solar soft X-ray flux, interplanetary magnetic field strength, $B_{t}$ , southward component of the interplanetary magnetic field, $B_{s}$ , solar wind speed, $V_{sw}$ , and the $y$ -component of the solar wind electric field, $E_{y}$ . We found only a weak correlation between the Dst of the geomagnetic storms associated with DC-FH-CMEs and the CME sky-plane speed and the CME direction parameter, while the correlation was strong between the Dst and all the solar wind parameters ( $B_{t}$ , $B_{s}$ , $V_{sw}$ , $E_{y}$ ) measured at 1 AU. We investigated the dependences of the properties of DC-FH-CMEs and the associated geomagnetic storms on different phases of solar cycles and the differences between Solar Cycles 23 and 24. In the rise phase of Solar Cycle 23 (SC23), five out of eight DC-FH-CMEs were geoeffective ( $\mbox{Dst} \leq- 50~\mbox{nT}$ ). In the corresponding phase of SC24, only four DC-FH-CMEs were observed, three of which were nongeoeffective ( $\mbox{Dst} > - 50~\mbox{nT}$ ). The largest number of DC-FH-CMEs occurred at the maximum phases of the cycles (21 and 17, respectively). Most of the storms with $\mbox{Dst}\leq- 100~\mbox{nT}$ occurred at or close to the maximum phases of the cycles. When comparing the storms during epochs of corresponding lengths in Solar Cycles 23 and 24, we found that during the first 85 months of Cycle 23 the geoeffectiveness rate of the disk-centre full-halo CMEs was 58% with an average minimum value of the Dst index of $- 146~\mbox{nT}$ . During the corresponding epoch of Cycle 24, only 35% of the disk-centre full-halo CMEs were geoeffective with an average value of Dst of $- 97~\mbox{nT}$ .
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- 2017
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23. The Energetic Particle Telescope: First Results
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Ghislain Grégoire, L. Bonnet, J. De Saedeleer, F. Preud’homme, E. Van Ransbeeck, G. Creve, Petteri Nieminen, D. Moreau, Sabrina Bonnewijn, D. Pauwels, Mathias Cyamukungu, Joseph Lemaire, A. Helderweirt, K. Litefti, G. Lopez Rosson, Viviane Pierrard, Eddy Neefs, C. Quevrin, Sylvie Benck, Eino Valtonen, Stanislav Borisov, B. Desoete, J. Cabrera, M. Anciaux, Risto Punkkinen, C. Semaille, Kris Borremans, Jeroen Maes, Wojtek Hajdas, and N. Brun
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Geomagnetic storm ,Physics ,Spectrometer ,Solar energetic particles ,Astrophysics::Instrumentation and Methods for Astrophysics ,Polar orbit ,Astronomy ,Astronomy and Astrophysics ,Atmospheric sciences ,law.invention ,South Atlantic Anomaly ,Telescope ,symbols.namesake ,Space and Planetary Science ,law ,Van Allen radiation belt ,Physics::Space Physics ,symbols ,Astrophysics::Solar and Stellar Astrophysics ,Satellite ,Astrophysics::Earth and Planetary Astrophysics ,Physics::Atmospheric and Oceanic Physics - Abstract
The Energetic Particle Telescope (EPT) is a new compact and modular ionizing particle spectrometer that was launched on 7 May 2013 to a LEO polar orbit at an altitude of 820 km onboard the ESA satellite PROBA-V. First results show electron, proton and helium ion fluxes in the South Atlantic Anomaly (SAA) and at high latitudes, with high flux increases during SEP (Solar Energetic Particles) events and geomagnetic storms. These observations help to improve the understanding of generation and loss processes associated to the Van Allen radiation belts.
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- 2014
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24. Investigation of the Geoeffectiveness of Disk-Centre Full-Halo Coronal Mass Ejections
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Dheyaa Ameri and Eino Valtonen
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- 2017
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25. Observations of solar energetic particle events during multiple coronal mass ejections
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Eino Valtonen, Silja Pohjolainen, and Firas Al-Hamadani
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Physics ,Coronal mass ejection ,Particle ,Astrophysics - Published
- 2016
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26. Resolving multiple sources of solar relativistic particles
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Andreas Klassen, Eino Valtonen, Leon Kocharov, and Ilya Usoskin
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Physics ,Physics::Space Physics ,Solar particle event ,Coronal mass ejection ,Astrophysics::Solar and Stellar Astrophysics ,Solar radius ,Neutron ,Electron ,Astrophysics ,Interplanetary spaceflight ,Event (particle physics) ,Relativistic particle - Abstract
We consider the time-profile morphology of solar high-energy particle emissions, including relativistic electrons in three energy channels of SOHO/EPHIN, relativistic protons as registered by the worldwide network of neutron monitors, and 100 MeV/n protons and helium in several energy channels of SOHO/ERNE. Based on numerical modeling of the interplanetary transport, we formulate a simple method for investigation of the high-energy particle sources operating at / near the Sun during the first hour of particle event. The method is applied to Ground Level Enhancement (GLE) and Solar Energetic Particle (SEP) events of the solar cycle 23. We conclude that depending on the GLE-SEP event scenario and detector vantage point, the observed particles originate from at least three sources. Possible nature of the sources is discussed in the framework of previous and new models of the high-energy particle production associated with global coronal (EIT) waves and CME shocks within about five solar radii from the Sun.
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- 2016
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27. Iron-rich solar particle events measured by SOHO/ERNE
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Osku Raukunen, Rami Vainio, and Eino Valtonen
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Physics ,Particle ,Astrophysics - Published
- 2016
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28. Solar energetic particle events related to disk-centre full-halo coronal mass ejections
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Dheyaa Ameri and Eino Valtonen
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Physics ,Coronal mass ejection ,Particle ,Astrophysics ,Halo - Published
- 2016
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29. High Statistics Measurement of the Positron Fraction in Primary Cosmic Rays of 0.5–500 GeV with the Alpha Magnetic Spectrometer on the International Space Station
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K. H. Guo, A. Lebedev, Dong-Chul Son, Y. Y. Fan, Massimo Gervasi, L. Tao, M. Capell, L. Accardo, C. Sbarra, Yun Shi, Antje Putze, B. Coste, I. Guerri, H. Jinchi, D. Haas, V. Vagelli, G. La Vacca, A. Malinin, A. Piluso, R. Pilastrini, I. Cernuda, I. Lazzizzera, Carlos Díaz, W. De Boer, David Maurin, E. Valente, M. Bourquin, Laurent Derome, D. Grandi, M. Xie, I. Gebauer, X. M. Qi, G. Schwering, J. Bazo, P. G. Rancoita, M. S. Krafczyk, Wei Li, C. Mañá, E. Fiandrini, J. C. Marin, W. Gillard, T. Urban, V. Choutko, B. Bertucci, W. H. Sun, Q. Meng, R. Q. Xiong, Franck Cadoux, P. Nunes, Teimuraz Lomtadze, Fabrizio Giulio Luca Pilo, C. Türkoʇlu, G. Castellini, M. Bizzarri, Won Kyu Calvin Sun, P. Goglov, Mayda Velasco, Federico Cindolo, W. Y. Jang, S. S. Vaurynovich, H. S. Chen, F. Spinella, V. Cascioli, Benjamin Monreal, N. Nikonov, Liqiu Wang, Veronica Bindi, Kwangsoo Kim, Chia-Hui Lin, M. J. Chae, C. Guandalini, M. Duranti, E. Pedreschi, G. Boella, Sadakazu Haino, E. Laudi, Y. J. Yu, Lucio Rossi, S. Xie, G. Coignet, M. Paniccia, Xiaoping Wang, G. Laurenti, S. Zeissler, D. Schuckardt, V. Poireau, Q. H. Ye, J. Gong, F. Giovacchini, Roald Z. Sagdeev, Luca Morescalchi, D. Aisa, C. Goy, R. J. García-López, F. Palmonari, S. Della Torre, X. W. Tang, M. Pauluzzi, Samuel C.C. Ting, Y. H. Chang, Zhixiang Tang, Fei Zhou, F. Massera, Arturo Alejandro Menchaca-Rocha, S. M. Schmidt, G. Ambrosi, V. Vitale, M. Orcinha, J. Q. Li, Valery Zhukov, J. P. Vialle, K. Bollweg, Gongming Xin, H. L. Li, Markus Battarbee, Paolo Zuccon, L. Di Masso, G. Gallucci, L. Basara, G. Volpini, R. Clavero, T. Siedenburg, A. Rozhkov, E. Finch, J. H. Zhang, Davide Rozza, S. Lim, I. Rodríguez, L. Farnesini, S. Borsini, Claudio Corti, A. Fiasson, Z. M. Zheng, A. Obermeier, K. Andeen, A. Contin, D. D'Urso, Mingming Yang, J. Feng, M. Pohl, Z. L. Weng, D. Rapin, V. Plyaskin, E. Postaci, Zheng Wang, X. Y. Shi, Philipp Azzarello, Matthias Heil, Mauro Tacconi, B. S. Shan, J. Casaus, M. Graziani, T. Kirn, G. M. Cheng, Matteo Boschini, J. Wienkenhöver, N. Masi, F. Luo, A. I. Chen, Zhiqi Huang, L. Barrin, M. B. Demirköz, A. Papi, Z. H. He, F. Nozzoli, C. Zurbach, A. Alvino, Hengchang Liu, P. Lipari, S. Bizzaglia, T. X. Li, Varlen Grabski, C. Pizzolotto, T. Eronen, X. Xia, C. Consolandi, A. Schulz von Dratzig, K. Kanishev, Yu. Galaktionov, Lin Cheng, Nicola Tomassetti, Z. Q. Yu, D. C. Mo, Y. Li, W. Xu, Roberto Battiston, J. Berdugo, K. C. Han, S. C. Lee, H. T. Lee, Dong Liu, Behcet Alpat, R. Pereira, Q. L. Wang, S. Di Falco, H. Yi, B. Borgia, F. Spada, J. J. Torsti, S. Pensotti, Antonino Zichichi, S. M. Ting, C. Delgado, S. Schael, A. Ghelfi, S. S. Lv, J. Hoffman, N. Attig, F. Cervelli, Zhijun Zhang, P. Mott, J. Sandweiss, Henning Gast, Tim Martin, Y. H. Shan, G. Scolieri, J. Q. Ni, C. H. Chung, A. Oliva, M. T. Zhang, U. Becker, Fernando Barão, J. S. Ricol, M. Behlmann, D. Cerreta, Ningsheng Xu, Thomas Lippert, C. Leluc, F. J. Eppling, B. Beischer, V. Bonnivard, H. Y. Chou, R. Henning, R. D. Majka, M. Dai, Z. Cui, O. Kounina, G. Rybka, M. Müller, H. Wu, P. Saouter, Peter H. Fisher, K. Luebelsmeyer, D. Tescaro, M. Aguilar, Ruiguang Wang, F. Dimiccoli, K. Whitman, E. Choumilov, R. Kossakowski, G. N. Kim, H. L. Zhuang, A. Barrau, M. J. Lu, A. Bartoloni, Bruce Rafael Mellado Garcia, Luísa Arruda, M. Lolli, C. P. Tang, S. Kunz, A. Eline, Timothy H. Hsieh, J. Y. Shi, J. Yang, A. Chikanian, Gianpaolo Carosi, Changgi Huh, J. Z. Luo, Z. Y. Li, Lucio Quadrani, M. Habiby, A. Bachlechner, X. B. Zhang, Eun-Suk Seo, Ying Lu, S. Rosier-Lees, V. Koutsenko, Eino Valtonen, Z. H. Li, Qiang Li, J. D. Burger, W. J. Du, K. Y. Wu, Manuela Vecchi, C. Vannini, P. von Doetinchem, X. D. Cai, Giuseppe Levi, G. Martinez, C. Palomares, C. Clark, Andrei Kounine, Q. Yan, G. Bigongiari, S. Caroff, N. Zimmermann, M. Incagli, Maria Ionica, Azzarello, Philipp, Bourquin, Maurice, Cadoux, Franck, Haas, Daniel, Habiby Alaoui, Marion, Leluc, Catherine, Li, Yang, Paniccia, Mercedes, Pohl, Martin, Rapin, Divic Jean, Saouter, Pierre, Accardo, L, Aguilar, M, Aisa, D, Alpat, B, Alvino, A, Ambrosi, G, Andeen, K, Arruda, L, Attig, N, Azzarello, P, Bachlechner, A, Barao, F, Barrau, A, Barrin, L, Bartoloni, A, Basara, L, Battarbee, M, Battiston, R, Bazo, J, Becker, U, Behlmann, M, Beischer, B, Berdugo, J, Bertucci, B, Bigongiari, G, Bindi, V, Bizzaglia, S, Bizzarri, M, Boella, G, de Boer, W, Bollweg, K, Bonnivard, V, Borgia, B, Borsini, S, Boschini, M, Bourquin, M, Burger, J, Cadoux, F, Cai, X, Capell, M, Caroff, S, Carosi, G, Casaus, J, Cascioli, V, Castellini, G, Cernuda, I, Cerreta, D, Cervelli, F, Chae, M, Chang, Y, Chen, A, Chen, H, Cheng, G, Cheng, L, Chikanian, A, Chou, H, Choumilov, E, Choutko, V, Chung, C, Cindolo, F, Clark, C, Clavero, R, Coignet, G, Consolandi, C, Contin, A, Corti, C, Coste, B, Cui, Z, Dai, M, Delgado, C, Della Torre, S, Demirköz, M, Derome, L, Di Falco, S, Di Masso, L, Dimiccoli, F, Díaz, C, von Doetinchem, P, Du, W, Duranti, M, D’Urso, D, Eline, A, Eppling, F, Eronen, T, Fan, Y, Farnesini, L, Feng, J, Fiandrini, E, Fiasson, A, Finch, E, Fisher, P, Galaktionov, Y, Gallucci, G, García, B, García López, R, Gast, H, Gebauer, I, Gervasi, M, Ghelfi, A, Gillard, W, Giovacchini, F, Goglov, P, Gong, J, Goy, C, Grabski, V, Grandi, D, Graziani, M, Guandalini, C, Guerri, I, Guo, K, Haas, D, Habiby, M, Haino, S, Han, K, He, Z, Heil, M, Henning, R, Hoffman, J, Hsieh, T, Huang, Z, Huh, C, Incagli, M, Ionica, M, Jang, W, Jinchi, H, Kanishev, K, Kim, G, Kim, K, Kirn, T, Kossakowski, R, Kounina, O, Kounine, A, Koutsenko, V, Krafczyk, M, Kunz, S, LA VACCA, G, Laudi, E, Laurenti, G, Lazzizzera, I, Lebedev, A, Lee, H, Lee, S, Leluc, C, Levi, G, Li, H, Li, J, Li, Q, Li, T, Li, W, Li, Y, Li, Z, Lim, S, Lin, C, Lipari, P, Lippert, T, Liu, D, Liu, H, Lolli, M, Lomtadze, T, Lu, M, Lu, Y, Luebelsmeyer, K, Luo, F, Luo, J, Lv, S, Majka, R, Malinin, A, Mañá, C, Marín, J, Martin, T, Martínez, G, Masi, N, Massera, F, Maurin, D, Menchaca Rocha, A, Meng, Q, Mo, D, Monreal, B, Morescalchi, L, Mott, P, Müller, M, Ni, J, Nikonov, N, Nozzoli, F, Nunes, P, Obermeier, A, Oliva, A, Orcinha, M, Palmonari, F, Palomares, C, Paniccia, M, Papi, A, Pauluzzi, M, Pedreschi, E, Pensotti, S, Pereira, R, Pilastrini, R, Pilo, F, Piluso, A, Pizzolotto, C, Plyaskin, V, Pohl, M, Poireau, V, Postaci, E, Putze, A, Quadrani, L, Qi, X, Rancoita, P, Rapin, D, Ricol, J, Rodríguez, I, Rosier Lees, S, Rossi, L, Rozhkov, A, Rozza, D, Rybka, G, Sagdeev, R, Sandweiss, J, Saouter, P, Sbarra, C, Schael, S, Schmidt, S, Schuckardt, D, Schulz von Dratzig, A, Schwering, G, Scolieri, G, Seo, E, Shan, B, Shan, Y, Shi, J, Shi, X, Shi, Y, Siedenburg, T, Son, D, Spada, F, Spinella, F, Sun, W, Tacconi, M, Tang, C, Tang, X, Tang, Z, Tao, L, Tescaro, D, Ting, S, Tomassetti, N, Torsti, J, Türkoğlu, C, Urban, T, Vagelli, V, Valente, E, Vannini, C, Valtonen, E, Vaurynovich, S, Vecchi, M, Velasco, M, Vialle, J, Vitale, V, Volpini, G, Wang, L, Wang, Q, Wang, R, Wang, X, Wang, Z, Weng, Z, Whitman, K, Wienkenhöver, J, Wu, H, Wu, K, Xia, X, Xie, M, Xie, S, Xiong, R, Xin, G, Xu, N, Xu, W, Yan, Q, Yang, J, Yang, M, Ye, Q, Yi, H, Yu, Y, Yu, Z, Zeissler, S, Zhang, J, Zhang, M, Zhang, X, Zhang, Z, Zheng, Z, Zhou, F, Zhuang, H, Zhukov, V, Zichichi, A, Zimmermann, N, Zuccon, P, Zurbach, C, L. Accardo, M. Aguilar, D. Aisa, B. Alpat, A. Alvino, G. Ambrosi, K. Andeen, L. Arruda, N. Attig, P. Azzarello, A. Bachlechner, F. Barao, A. Barrau, L. Barrin, A. Bartoloni, L. Basara, M. Battarbee, R. Battiston, J. Bazo, U. Becker, M. Behlmann, B. Beischer, J. Berdugo, B. Bertucci, G. Bigongiari, V. Bindi, S. Bizzaglia, M. Bizzarri, G. Boella, W. d. Boer, K. Bollweg, V. Bonnivard, B. Borgia, S. Borsini, M. J. Boschini, M. Bourquin, J. Burger, F. Cadoux, X. D. Cai, M. Capell, S. Caroff, G. Carosi, J. Casau, V. Cascioli, G. Castellini, I. Cernuda, D. Cerreta, F. Cervelli, M. J. Chae, Y. H. Chang, A. I. Chen, H. Chen, G. M. Cheng, H. S. Chen, L. Cheng, A. Chikanian, H. Y. Chou, E. Choumilov, V. Choutko, C. H. Chung, F. Cindolo, C. Clark, R. Clavero, G. Coignet, C. Consolandi, A. Contin, C. Corti, B. Coste, Z. Cui, M. Dai, C. Delgado, S. D. Torre, M. B. Demirkoz, L. Derome, S. D. Falco, L. D. Masso, F. Dimiccoli, C. Diaz, P. v. Doetinchem, W. J. Du, M. Duranti, D. D'Urso, A. Eline, F. J. Eppling, T. Eronen, Y. Y. Fan, L. Farnesini, J. Feng, E. Fiandrini, A. Fiasson, E. Finch, P. Fisher, Y. Galaktionov, G. Gallucci, B. Garcia, R. Garcia-Lopez, H. Gast, I. Gebauer, M. Gervasi, A. Ghelfi, W. Gillard, F. Giovacchini, P. Goglov, J. Gong, C. Goy, V. Grabski, D. Grandi, M. Graziani, C. Guandalini, I. Guerri, K. H. Guo, D. Haa, M. Habiby, S. Haino, K. C. Han, Z. H. He, M. Heil, R. Henning, J. Hoffman, T. H. Hsieh, Z. C. Huang, C. Huh, M. Incagli, M. Ionica, W. Y. Jang, H. Jinchi, K. Kanishev, G. N. Kim, K. S. Kim, T. Kirn, R. Kossakowski, O. Kounina, A. Kounine, V. Koutsenko, M. S. Krafczyk, S. Kunz, G. L. Vacca, E. Laudi, G. Laurenti, I. Lazzizzera, A. Lebedev, H. T. Lee, S. C. Lee, C. Leluc, G. Levi, H. L. Li, J. Q. Li, Q. Li, T. X. Li, W. Li, Y. Li, Z. H. Li, Z. Y. Li, S. Lim, C. H. Lin, P. Lipari, T. Lippert, D. Liu, H. Liu, M. Lolli, T. Lomtadze, M. J. Lu, Y. S. Lu, K. Luebelsmeyer, F. Luo, J. Z. Luo, S. S. Lv, R. Majka, A. Malinin, C. Mana, J. Marin, T. Martin, G. Martinez, N. Masi, F. Massera, D. Maurin, A. Menchaca-Rocha, Q. Meng, D. C. Mo, B. Monreal, L. Morescalchi, P. Mott, M. Muller, J. Q. Ni, N. Nikonov, F. Nozzoli, P. Nune, A. Obermeier, A. Oliva, M. Orcinha, F. Palmonari, C. Palomare, M. Paniccia, A. Papi, M. Pauluzzi, E. Pedreschi, S. Pensotti, R. Pereira, R. Pilastrini, F. Pilo, A. Piluso, C. Pizzolotto, V. Plyaskin, M. Pohl, V. Poireau, E. Postaci, A. Putze, L. Quadrani, X. M. Qi, P. G. Rancoita, D. Rapin, J. S. Ricol, I. Rodriguez, S. Rosier-Lee, L. Rossi, A. Rozhkov, D. Rozza, G. Rybka, R. Sagdeev, J. Sandwei, P. Saouter, C. Sbarra, S. Schael, S. M. Schmidt, D. Schuckardt, A. S. von, G. Schwering, G. Scolieri, E. S. Seo, B. S. Shan, Y. H. Shan, J. Y. Shi, X. Y. Shi, Y. M. Shi, T. Siedenburg, D. Son, F. Spada, F. Spinella, W. Sun, W. H. Sun, M. Tacconi, C. P. Tang, X. W. Tang, Z. C. Tang, L. Tao, D. Tescaro, S. C. C., S. M. Ting, N. Tomassetti, J. Torsti, C. Turkoglu, T. Urban, V. Vagelli, E. Valente, C. Vannini, E. Valtonen, S. Vaurynovich, M. Vecchi, M. Velasco, J. P. Vialle, V. Vitale, G. Volpini, L. Q. Wang, Q. L. Wang, R. S. Wang, X. Wang, Z. X. Wang, Z. L. Weng, K. Whitman, J. Wienkenhover, H. Wu, K. Y. Wu, X. Xia, M. Xie, S. Xie, R. Q. Xiong, G. M. Xin, N. S. Xu, W. Xu, Q. Yan, J. Yang, M. Yang, Q. H. Ye, H. Yi, Y. J. Yu, Z. Q. Yu, S. Zeissler, J. H. Zhang, M. T. Zhang, X. B. Zhang, Z. Zhang, Z. M. Zheng, F. Zhou, H. L. Zhuang, V. Zhukov, A. Zichichi, N. Zimmermann, P. Zuccon, C. Zurbach, Istituto Nazionale di Fisica Nucleare, Sezione di Perugia (INFN, Sezione di Perugia), Istituto Nazionale di Fisica Nucleare (INFN), Centro de Investigaciones Energéticas Medioambientales y Tecnológicas [Madrid] (CIEMAT), Institut für Experimentelle Kernphysik [Karlsruhe] (EKP), Karlsruher Institut für Technologie (KIT), Jülich Aachen Research Alliance (JARA), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), CERN [Genève], Istituto Nazionale di Fisica Nucleare, Sezione di Roma 3 (INFN, Sezione di Roma 3), 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), University of Turku, Massachusetts Institute of Technology (MIT), INFN Sezione di Pisa (INFN Sezione di Pisa), University of Hawai'i [Honolulu] (UH), Istituto Nazionale di Fisica Nucleare, Sezione di Milano (INFN), Karlsruhe Institute of Technology (KIT), NASA Johnson Space Center (JSC), NASA, Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Département de Physique Nucléaire et Corpusculaire [Genève] (DPNC), Université de Genève (UNIGE), Istituto Nazionale di Ottica [Firenze] (INO-CNR), Consiglio Nazionale delle Ricerche (CNR), Istituto Nazionale di Fisica Nucleare [Pisa] (INFN), EWHA Womans University (EWHA), National Central University [Taiwan] (NCU), Academia Sinica, Istituto Nazionale di Fisica Nucleare, Sezione di Bologna (INFN, Sezione di Bologna), Laboratoire Univers et Particules de Montpellier (LUPM), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), and AMS
- Subjects
Astrophysics and Astronomy ,[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,Astrophysics::High Energy Astrophysical Phenomena ,General Physics and Astronomy ,cosmic rays studies ,Cosmic ray ,Electron ,ddc:500.2 ,7. Clean energy ,Space mission ,[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,Nuclear physics ,Physics and Astronomy (all) ,FIS/05 - ASTRONOMIA E ASTROFISICA ,Positron ,International Space Station ,Alpha Magnetic Spectrometer ,ddc:550 ,Dark matter ,ASTROPARTICLE PHYSICS ,AMS ,Cosmic rays ,Positron fraction ,antimatter and dark matter ,positrons ,Physics ,Range (particle radiation) ,ta115 ,Magnetic spectrometer ,ELECTRONS ,Cosmic rays, Positron fraction, International Space Station ,FIS/01 - FISICA SPERIMENTALE ,Physics::Accelerator Physics ,Satellite ,High Energy Physics::Experiment ,Particle Physics - Experiment ,Energy (signal processing) - Abstract
A precision measurement by AMS of the positron fraction in primary cosmic rays in the energy range from 0.5 to 500 GeV based on 10.9 million positron and electron events is presented. This measurement extends the energy range of our previous observation and increases its precision. The new results show, for the first time, that above ∼200 GeV the positron fraction no longer exhibits an increase with energy.
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- 2016
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30. Observation of solar energetic particle (SEP) events associated with narrow CMEs
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A. Al-Sawad, W. Al-Ramdhan, H. Allawi, and Eino Valtonen
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Physics ,Range (particle radiation) ,Physics and Astronomy (miscellaneous) ,Proton ,Solar flare ,Astronomy ,Astronomy and Astrophysics ,Electron ,Astrophysics ,law.invention ,Path length ,law ,Observatory ,Physics::Space Physics ,Astrophysics::Solar and Stellar Astrophysics ,Event (particle physics) ,Flare - Abstract
We report here on two proton energetic particle events observed by the Energetic and Relativistic Nuclei and Electron (ERNE) instrument on the Solar and Heliospheri- cal Observatory (SOHO). Both events were impulsive (SEP) events with intensities of > 10 3 cm 2 sr 1 s 1 MeV 1 at an energy range of tens of MeVs and were associated with CMEs of angular widths 800 kms 1 . In one of the events there was no associated solar flare, which indicates that the first injected protons were completely due to the associated CME and in the second event the associated solar flare was an impulsive M1.1 class flare and the calculated first injection time for protons of en- ergies 36 MeV and propagating along 1.2 AU path length, was close to the liftoff time of the CME. These observations are inconsistent with the view presented in some studies that narrow fast CME are not associated with SEP events.
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- 2012
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31. OBSERVED CORE OF A GRADUAL SOLAR ENERGETIC PARTICLE EVENT
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Andreas Klassen, Barbara J. Thompson, Leon Kocharov, Eino Valtonen, and M. J. Reiner
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Physics ,education.field_of_study ,Solar energetic particles ,Solar flare ,Astrophysics::High Energy Astrophysical Phenomena ,Population ,Coronal cloud ,Astronomy ,Astronomy and Astrophysics ,Magnetic reconnection ,Astrophysics ,Solar wind ,Space and Planetary Science ,Physics::Space Physics ,Physics::Atomic and Molecular Clusters ,Coronal mass ejection ,Astrophysics::Solar and Stellar Astrophysics ,Bow shock (aerodynamics) ,education - Abstract
Using space-borne particle and EUV detection and radio spectrograms from both ground-based and space-borne instruments, we study the first phase of the major solar energetic particle (SEP) event associated with the western solar flare and fast and wide coronal mass ejection (CME) on 2000 April 4. The SEP event being observed at the magnetic connection to the eruption's center starts with deka-MeV nucl–1 helium- and relativistic electron-rich production from coronal sources identified with the electromagnetic diagnostics and the SEP event modeling. The broadband observations and modeling of the initial phase of the "well-connected" major SEP event support the idea that acceleration of SEPs starts in the helium-rich plasma of the eruption's core in association with coronal shocks and magnetic reconnections caused by the CME liftoff, and that the coronal component dominates during the first hour of the SEP event considered, not yet being shielded by the CME bow shock in the solar wind. The first phase of the SEP event is followed by a second phase of SEP production associated with a decelerating CME-driven shock wave in the solar wind, which accelerates ions from a distinct, helium-poor seed particle population that may originate from the CME interaction with a coronal streamer.
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- 2010
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32. Solar Intensity X-ray and particle Spectrometer (SIXS)
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J. Peltonen, M. Roos, P. Portin, Manuel Grande, Hans Andersson, M. Anttila, Rami Vainio, Mark L. Prydderch, M. Syrjasuo, G.W. Fraser, L. Alha, Juhani Huovelin, Hannu Koskinen, Karri Muinonen, M. Kato, J. Lehti, Eino Valtonen, M. Talvioja, T. Vihavainen, Jyri Näränen, E. Kiuru, Walter Schmidt, and A. Malkki
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010504 meteorology & atmospheric sciences ,Astrophysics::High Energy Astrophysical Phenomena ,chemistry.chemical_element ,Electron ,Scintillator ,01 natural sciences ,7. Clean energy ,Particle detector ,Optics ,0103 physical sciences ,Particle radiation ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences ,Physics ,Spectrometer ,Solar energetic particles ,business.industry ,Bremsstrahlung ,Astronomy and Astrophysics ,Mercury (element) ,chemistry ,13. Climate action ,Space and Planetary Science ,Physics::Space Physics ,Astrophysics::Earth and Planetary Astrophysics ,business - Abstract
The Solar Intensity X-ray and particle Spectrometer (SIXS) on the BepiColombo Mercury Planetary Orbiter (MPO) will investigate the direct solar X-rays, and energetic protons and electrons which pass the Spacecraft on their way to the surface of Mercury. These measurements are vitally important for understanding quantitatively the processes that make Mercury's surface glow in X-rays, since all X-rays from Mercury are due to interactions of the surface with incoming highly energetic photons and space particles. The X-ray emission of Mercury's surface will be analysed to understand its structure and composition. SIXS data will also be utilised for studies of the solar X-ray corona, flares, solar energetic particles, and the magnetosphere of Mercury, and for providing information on solar eruptions to other BepiColombo instruments. SIXS consists of two detector subsystems. The X-ray detector system includes three identical GaAs PIN detectors which measure the solar spectrum at 1–20 keV energy range, and their combined field-of-view covers ∼1/4 of the whole sky. The particle detector system consists of an assembly including a cubic central CsI(Tl) scintillator detector with five of its six surfaces covered by a thin Si detector, which together perform low-resolution particle spectroscopy with a rough angular resolution over a field-of-view covering ∼1/4 of the whole sky. The energy range of detected particle spectra is 0.1–3 MeV for electrons and 1–30 MeV for protons. A major task for the SIXS instrument is the measurement of solar X-rays on the dayside of Mercury's surface to enable modeling of X-ray fluorescence and scattering on the planet's surface. Since highly energetic particles are expected to also induce a significant amount of X-ray emission via particle-induced X-ray emission (PIXE) and bremsstrahlung when they are absorbed by the solid surface of the planet Mercury, SIXS performs measurements of fluxes and spectra of protons and electrons. SIXS performs particle measurement at all orbital phases of the MPO as the particle radiation can occur also on the night side of Mercury. The energy ranges, resolutions, and timings of X-ray and particle measurements by SIXS have been adjusted to match with the requirements for interpretation of data from Mercury's surface, to be performed by utilising the data of the Mercury Imaging X-ray Spectrometer (MIXS), which will measure X-ray emission from the surface.
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- 2010
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33. History of cosmic ray research in Finland
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Ilya Usoskin, Rami Vainio, Eino Valtonen, A.M. Aurela, and P. Tanskanen
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Physics ,Atmospheric Science ,Neutron monitor ,Research groups ,010504 meteorology & atmospheric sciences ,Aerospace Engineering ,Astronomy and Astrophysics ,Cosmic ray ,Astrophysics ,01 natural sciences ,law.invention ,Telescope ,Geophysics ,Space and Planetary Science ,law ,0103 physical sciences ,Fully automatic ,General Earth and Planetary Sciences ,Space Science ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences - Abstract
The history of cosmic ray research in Finland can be traced back to the end of 1950s, when first ground-based cosmic ray measurements started in Turku. The first cosmic ray station was founded in Oulu in 1964 performing measurements of cosmic rays by a muon telescope, which was later complemented by a neutron monitor. Since the 1990s, several research centers and universities, such as The Finnish Meteorological Institute, Helsinki University of Technology, University of Oulu, University of Turku and University of Helsinki have been involved in space science projects, such as SOHO, AMS, Cluster, Cassini, BepiColombo, etc. At the same time, ground-based cosmic ray measurements have reached a new level, including a fully automatic on-line database in Oulu and a new muon measuring underground site in Pyhasalmi. Research groups in Helsinki, Oulu and Turku have also extensive experience in theoretical investigations of different aspects of cosmic ray physics. Cosmic ray research has a 50-year long history in Finland, covering a wide range from basic long-running ground-based observations to high-technology space-borne instrumentation and sophisticated theoretical studies. Several generations of researchers have been involved in the study ensuring transfer of experience and building the recognized Finnish research school of cosmic ray studies.
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- 2009
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34. Radiation Tolerance Tests of Small-Sized CsI(Tl) Scintillators Coupled to Photodiodes
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S. Nenonen, Rami Vainio, O. V. Dudnik, Ari Virtanen, Hans Andersson, Heikki Kettunen, Juhani Huovelin, A. M. Kudin, Mikko Rossi, J. Peltonen, Eino Valtonen, E.V. Kurbatov, Yu.A. Borodenko, T. Eronen, and J. Lehti
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Nuclear and High Energy Physics ,010504 meteorology & atmospheric sciences ,Silicon ,Tolerance analysis ,Physics::Instrumentation and Detectors ,Physics::Medical Physics ,chemistry.chemical_element ,Scintillator ,01 natural sciences ,7. Clean energy ,Fluence ,030218 nuclear medicine & medical imaging ,law.invention ,03 medical and health sciences ,0302 clinical medicine ,Radiation tolerance ,law ,Electrical and Electronic Engineering ,Nuclear Experiment ,0105 earth and related environmental sciences ,Physics ,business.industry ,Photodiode ,Nuclear Energy and Engineering ,chemistry ,Scintillation counter ,Optoelectronics ,Degradation (geology) ,business - Abstract
Radiation tolerance of small-sized CsI (Tl) crystals coupled to silicon photodiodes was studied by using protons. Irradiations up to the fluence of 1012 protons/cm2 were used. Degradation of light output by less than 5% was achieved.
- Published
- 2009
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35. GRADUAL SOLAR ENERGETIC PARTICLE EVENT ASSOCIATED WITH A DECELERATING SHOCK WAVE
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M. J. Reiner, Timo Laitinen, O. Saloniemi, A. Al-Sawad, Leon Kocharov, and Eino Valtonen
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Shock wave ,Physics ,Shock (fluid dynamics) ,Astrophysics::High Energy Astrophysical Phenomena ,Astronomy ,Astronomy and Astrophysics ,Electron ,Astrophysics ,Solar wind ,Space and Planetary Science ,Observatory ,Physics::Space Physics ,Coronal mass ejection ,Astrophysics::Solar and Stellar Astrophysics ,Interplanetary magnetic field ,Event (particle physics) - Abstract
On 2000 April 4-6 the Energetic and Relativistic Nuclei and Electron particle telescope on the Solar and Heliospheric Observatory spacecraft observed a major solar energetic particle (SEP) event associated with two coronal mass ejections (CMEs) separated by approximately 8 hr. The first CME was accompanied by a low-frequency type II radio burst observed by the WAVES receivers on the Wind spacecraft. Analysis of the high-precision measurements of the {approx}20 MeV proton flux anisotropy, model fitting of the type II dynamic spectrum, and SEP transport modeling support the idea that the shock wave of the first CME was an efficient accelerator for {approx}20 MeV protons during only the first 6 hr after the launch. This shock gradually slowed down, weakened, and became transparent for the protons produced by the second eruption behind the previous CME. The main production of SEPs due to the two successive eruptions continued together for 12 hr. The near-Earth SEP event was additionally amplified by the SEP mirroring in the interplanetary magnetic field draping at the edge of an old CME beyond the Earth's orbit, which made the SEP intensity-time profiles more prolonged than would be expected based on the assumption of SEP transport in the standardmore » solar wind.« less
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- 2009
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36. Solar energetic particle fluences from SOHO/ERNE
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E. Riihonen, Eino Valtonen, and Iiro-Ville Lehtinen
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Nuclear physics ,Physics ,Range (particle radiation) ,Geophysics ,chemistry ,Solar energetic particles ,Total dose ,chemistry.chemical_element ,Particle ,Space weather ,Atomic physics ,Fluence ,Helium - Abstract
We have calculated integral fluences of solar protons and helium nuclei at 19 energy thresholds between 1.6 and 90 MeV/n from the SOHO/ERNE measurements during the years 1996–2005. We have also calculated fluences of oxygen and iron in the energy range from 10 up to a few hundred MeV/n for nineteen solar energetic particle (SEP) events. These are the first results of the work aiming at a full employment of the ERNE data in investigating the fluence distributions of SEP events over the entire solar activity cycle 23 and in deriving the total dose received on-board SOHO during its mission. Some instrumental problems are identified and future developments are presented.
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- 2008
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37. A New Approach to Interplanetary Transport of Solar Energetic Particles in Impulsive Events
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Victor J. Pizzo, Eino Valtonen, R. D. Zwickl, and L. Kocharov
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Physics ,Solar energetic particles ,Astrophysics::High Energy Astrophysical Phenomena ,Coronal hole ,Flux ,Astronomy and Astrophysics ,Atmospheric sciences ,Wind speed ,Computational physics ,Solar wind ,Space and Planetary Science ,Physics::Space Physics ,Coronal mass ejection ,Astrophysics::Solar and Stellar Astrophysics ,Magnetopause ,Astrophysics::Earth and Planetary Astrophysics ,Interplanetary spaceflight - Abstract
Impulsive,3He-rich events originate close to the interface between slow solar wind overlying active regions and a faster solar wind coming from small coronal holes. This causes large-scale magnetic compressions to be an interplanetary environment for solar energetic particle (SEP) transport in impulsive events, which is typically ignored by SEP modelers. We have modeled SEP transport in a simplified corotating solar wind structure to estimate the possible effect of the rising wind speed on particle anisotropy and spectra at 1 AU. Along with traditional modeling of SEP transport in the static magnetic field and the field-aligned solar wind flow of the corotating frame of reference, we have formulated and tested a new model that is the first model of focused transport applicable to a general case of SEP propagation in realistic, dynamic, and structured solar wind. Numerical modeling shows that a fast increase of the wind speed by only 200 km s−1 can strongly affect the SEP flux anisotropy at 1 AU. Accurate analysis of impulsive SEP events can be done with the use of solar wind data, SEP flux anisotropy measurements, and the new approach that accounts for the solar wind structures associated with the sources of impulsive events and uses the general solution of the focused transport problem applicable to SEPs in realistic solar wind.
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- 2008
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38. Sources of SEP Acceleration during a Flare – CME Event
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Rami Vainio, A. Hillaris, Silja Pohjolainen, N. J. Lehtinen, K. Huttunen-Heikinmaa, and Eino Valtonen
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010504 meteorology & atmospheric sciences ,Astrophysics::High Energy Astrophysical Phenomena ,Frequency drift ,FOS: Physical sciences ,Electron ,Astrophysics ,7. Clean energy ,01 natural sciences ,Radio spectrum ,law.invention ,Magnetogram ,law ,0103 physical sciences ,Coronal mass ejection ,Astrophysics::Solar and Stellar Astrophysics ,Bow shock (aerodynamics) ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences ,Physics ,Astrophysics (astro-ph) ,Astronomy and Astrophysics ,13. Climate action ,Space and Planetary Science ,Physics::Space Physics ,Interplanetary spaceflight ,Flare - Abstract
A high-speed halo-type coronal mass ejection (CME), associated with a GOES M4.6 soft X-ray flare in NOAA AR 0180 at S12W29 and an EIT wave and dimming, occurred on 9 November 2002. A complex radio event was observed during the same period. It included narrow-band fluctuations and frequency-drifting features in the metric wavelength range, type III burst groups at metric--hectometric wavelengths, and an interplanetary type II radio burst, which was visible in the dynamic radio spectrum below 14 MHz. To study the association of the recorded solar energetic particle (SEP) populations with the propagating CME and flaring, we perform a multi-wavelength analysis using radio spectral and imaging observations combined with white-light, EUV, hard X-ray, and magnetogram data. Velocity dispersion analysis of the particle distributions (SOHO and Wind in situ observations) provides estimates for the release times of electrons and protons. Our analysis indicates that proton acceleration was delayed compared to the electrons. The dynamics of the interplanetary type II burst identify the burst source as a bow shock created by the fast CME. The type III burst groups, with start times close to the estimated electron release times, trace electron beams travelling along open field lines into the interplanetary space. The type III bursts seem to encounter a steep density gradient as they overtake the type II shock front, resulting in an abrupt change in the frequency drift rate of the type III burst emission. Our study presents evidence in support of a scenario in which electrons are accelerated low in the corona behind the CME shock front, while protons are accelerated later, possibly at the CME bow shock high in the corona., Solar Physics, November 2007, in press
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- 2007
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39. Correcting for interplanetary scattering in velocity dispersion analysis of solar energetic particles
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K. Huttunen-Heikinmaa, Eino Valtonen, Timo Laitinen, and Silvia Dalla
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Physics ,010504 meteorology & atmospheric sciences ,Solar energetic particles ,Scattering ,Monte Carlo method ,Velocity dispersion ,FOS: Physical sciences ,Astronomy and Astrophysics ,F500 ,01 natural sciences ,Space Physics (physics.space-ph) ,Computational physics ,Path length ,Astrophysics - Solar and Stellar Astrophysics ,Physics - Space Physics ,Space and Planetary Science ,0103 physical sciences ,Physics::Space Physics ,Particle ,Heliospheric current sheet ,010303 astronomy & astrophysics ,Event (particle physics) ,Solar and Stellar Astrophysics (astro-ph.SR) ,0105 earth and related environmental sciences - Abstract
To understand the origin of Solar Energetic Particles (SEPs), we must study their injection time relative to other solar eruption manifestations. Traditionally the injection time is determined using the Velocity Dispersion Analysis (VDA) where a linear fit of the observed event onset times at 1 AU to the inverse velocities of SEPs is used to derive the injection time and path length of the first-arriving particles. VDA does not, however, take into account that the particles that produce a statistically observable onset at 1 AU have scattered in the interplanetary space. We use Monte Carlo test particle simulations of energetic protons to study the effect of particle scattering on the observable SEP event onset above pre-event background, and consequently on VDA results. We find that the VDA results are sensitive to the properties of the pre-event and event particle spectra as well as SEP injection and scattering parameters. In particular, a VDA-obtained path length that is close to the nominal Parker spiral length does not imply that the VDA injection time is correct. We study the delay to the observed onset caused by scattering of the particles and derive a simple estimate for the delay time by using the rate of intensity increase at the SEP onset as a parameter. We apply the correction to a magnetically well-connected SEP event of June 10 2000, and show it to improve both the path length and injection time estimates, while also increasing the error limits to better reflect the inherent uncertainties of VDA., 10 pages, 9 figures; Accepted for publication in Astrophysical Journal
- Published
- 2015
40. Proton and helium release times in SEP events observed with SOHO/ERNE
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Eino Valtonen, Timo Laitinen, and K. Huttunen-Heikinmaa
- Subjects
Physics ,Proton ,Significant difference ,chemistry.chemical_element ,Velocity dispersion ,Astronomy and Astrophysics ,Astrophysics ,law.invention ,Intensity (physics) ,Nuclear physics ,Particle acceleration ,chemistry ,Space and Planetary Science ,law ,Coronal mass ejection ,Helium ,Flare - Abstract
We determine the proton and helium nuclei release times at the Sun for 25 SEP events within the time period May 8, 1996-June 20, 2001, and compare them to each other. The event onset times at 1 AU are determined with a Poisson-CUSUM method, and the solar release times are obtained by the velocity dispersion analysis. Velocity dispersions were derived in the energy range 14-51 MeV/n. If the release times of protons and helium nuclei do not overlap within their error limits, and if protons are released earlier than helium, then the helium event is defined as “delayed”. Seventeen helium events (68%) were found to be “delayed” and only eight (32%) “non-delayed”. The average delay was () minutes. The event-related flare location had an important role in the “non-delayed” events. A significant difference was found in the helium-to-proton ratios at the time of maximum intensity of the “delayed” and “non-delayed” events. No clear evidence was found that the “delayed” and “non-delayed” events would correspond the classical gradual-impulsive division of SEP events. We find that the delay is related to the poor magnetic connection between the flare site and the spacecraft.
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- 2005
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41. Energetic particle signatures of geoeffective coronal mass ejections
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Timo Laitinen, K. Huttunen-Heikinmaa, and Eino Valtonen
- Subjects
Physics ,Geomagnetic storm ,Atmospheric Science ,Solar energetic particles ,Aerospace Engineering ,Astronomy ,Astronomy and Astrophysics ,Transit time ,Storm ,Physics::Geophysics ,Geophysics ,Space and Planetary Science ,Physics::Space Physics ,Coronal mass ejection ,Astrophysics::Solar and Stellar Astrophysics ,General Earth and Planetary Sciences ,Halo ,Interplanetary spaceflight - Abstract
We have studied statistically associations of moderate and intense geomagnetic storms with coronal mass ejections (CMEs) and energetic particle events. The goal was to identify specific energetic particle signatures, which could be used to improve the predictions of the geoeffectiveness of full and partial halo CMEs. Protons in the range 1–110 MeV from the ERNE experiment onboard SOHO are used in the analysis. The study covers the time period from August 1996 to July 2000. We demonstrate the feasibility of energetic particle observations as an additional source of information in evaluating the geoeffectiveness of full and partial halo CMEs. Based on the observed onset times of solar energetic particle (SEP) events and energetic storm particle (ESP) events, we derive a proxy for the transit times of shocks driven by the interplanetary counterparts of coronal mass ejections from the Sun to the Earth. For a limited number of geomagnetic storms which can be associated to both SEP and ESP signatures, we found that this transit time correlates with the strength of geomagnetic storms.
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- 2005
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42. Precision Measurement of the Helium Flux in Primary Cosmic Rays of Rigidities 1.9 GV to 3 TV with the Alpha Magnetic Spectrometer on the International Space Station
- Author
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N. Nikonov, Corrado Gargiulo, A. Egorov, I. Cernuda, Carlos Díaz, W. De Boer, Corinne Goy, Wei Sun, Haifeng Li, P. Vialle, E. Fiandrini, H. S. Chen, Zhiqi Huang, Xiaoqun Wang, I. Gebauer, C. Türkoğlu, Arturo Alejandro Menchaca-Rocha, S. Krafczyk, L. Tao, S. Xie, J. Q. Ni, Fabrizio Giulio Luca Pilo, F. Spinella, S. S. Lv, Maria Ionica, S. Chen, Markus Battarbee, J. Gong, J. Sandweiss, H. Y. Chou, R. D. Majka, S. Wang, Z. Q. Yu, O. Kounina, Paolo Zuccon, Samuel C.C. Ting, H. Yi, H. Wu, Z. Cui, W. Tang, H. Shan, M. Qi, Matthias Heil, E. Finch, J. H. Zhang, S. Zhang, W. Creus, G. Laurenti, T. J. N. Nelson, E. Valente, M. Paniccia, A. Von Dratzig, Davide Rozza, K. Andeen, L. Farnesini, I. Rodríguez, Chuanguo Zhang, Z. L. Weng, D. Rapin, V. Plyaskin, A. Lebedev, A. Papi, Dong-Chul Son, P. Tang, J. W. Song, J. Wienkenhöver, Andrea Contin, Hengchang Liu, S. Lim, H. Sun, Philipp Azzarello, N. Masi, F. Luo, L. Barrin, Z. Qu, M. Willenbrock, J. J. Torsti, S. Pensotti, G. La Vacca, Mauro Tacconi, Roald Z. Sagdeev, Yang Yang, G. Schwering, Antonino Zichichi, G. Coignet, David Maurin, Xin Wu, J. Eppling, S. Della Torre, M. Crispoltoni, S. Rosier-Lees, J. Casaus, L. Qu, Chung-Cherng Lin, Teimuraz Lomtadze, M. B. Demirköz, C. Han, Henning Gast, M. Aguilar, Matteo Boschini, Chau-Hwang Lee, J. Berdugo, A. Fiasson, F. Dimiccoli, Wei Li, Laurent Derome, A. Bartoloni, X. Xia, C. Pizzolotto, R. J. García-López, Y. Fan, E. Choumilov, J. C. Marin, V. Poireau, Xubo Qin, P. Mott, Yun Shi, R. Kossakowski, Franck Cadoux, P. Nunes, A. Rozhkov, F. Spada, Lin Cheng, N. Picot-Clemente, F. Palmonari, M. Bourquin, C. Ting, L. Di Masso, M. Bizzarri, M. Duranti, E. Pedreschi, L. Basara, U. Becker, C. H. Chung, Xinxin Li, Y. J. Yu, S. Zeissler, Yu. Galaktionov, D. Aisa, I. Guerri, G. Boella, Varlen Grabski, M. Vecchi, Massimo Gervasi, Dong Liu, Z. Luo, Thomas Lippert, S. Q. Lu, Mayda Velasco, Valery Zhukov, M. T. Zhang, S. Vitillo, Z. M. Zheng, Fernando Barão, M. Pauluzzi, Bruce Rafael Mellado Garcia, Z. H. He, A. I. Chen, V. Vitale, F. Nozzoli, H. Jinchi, M. Behlmann, T. Siedenburg, A. Piluso, D. Cerreta, A. Ghelfi, M. Capell, Claudio Corti, Ningsheng Xu, G. Ambrosi, S. Caroff, J. Hoffman, T. Eronen, R. Clavero, D. Grandi, W. Xu, Naihua Wang, F. Cervelli, A. Obermeier, E. Gil, P. Lipari, T. Räihä, P. Goglov, I. Lazzizzera, M. Pohl, B. Bertucci, M. Xie, H. Ye, C. Mañá, Veronica Bindi, G. Scolieri, Nicola Tomassetti, Shihao Zhang, Hsiang Szu Chang, Behcet Alpat, Luísa Arruda, Antje Putze, T. Kirn, D. Haas, V. Vagelli, Shinhong Kim, C. Mo, Pier-Giorgio Rancoita, Q. Meng, Sadakazu Haino, H. L. Zhuang, A. Barrau, S. J. Schmidt, Q. L. Wang, C. Delgado, T. Urban, V. Choutko, A. Korkmaz, S. Seo, M. J. Chae, C. Guandalini, R. Pereira, M. Chen, K. Bollweg, Miaoran Lu, Zheng Wang, M. Habiby, B. Coste, M. Graziani, V. Formato, Horngming Hsieh, M. Incagli, K. Whitman, Ju Li, Roberto Battiston, B. Borgia, J. Yang, H. Guo, M. Müller, Changgi Huh, Zhijun Zhang, P. Saouter, S. Di Falco, Peter H. Fisher, Tim Martin, F. Giovacchini, Luca Morescalchi, Q. Xiong, K. Luebelsmeyer, Zhixiang Tang, M. Orcinha, A. Alvino, C. Vannini, S. Shan, P. von Doetinchem, N. Kim, X. D. Cai, F. Donnini, N. Attig, Hyun Lee, Andrei Kounine, Q. Yan, N. Zimmermann, S. Borsini, G. Castellini, J. Feng, G. Martinez, C. Palomares, C. Clark, S. Schael, C. Consolandi, Elisa Laudi, J. D. Burger, S. S. Vaurynovich, D. Tescaro, Yongyao Li, Mingming Yang, A. Oliva, D. D'Urso, C. Leluc, G. Gallucci, Yaomin Dai, B. Beischer, V. Bonnivard, K. Kanishev, S. Bizzaglia, Y. Jang, A. Bachlechner, X. B. Zhang, J. Bazo, V. Koutsenko, Eino Valtonen, Z. H. Li, Qiang Li, S. Ricol, M. Lolli, A. Eline, Massachusetts Institute of Technology. Department of Physics, Massachusetts Institute of Technology. Laboratory for Nuclear Science, Becker, Ulrich J., Behlmann, Matthew Daniel, Burger, Joseph D., Cai, Xudong, Capell, Michael H., Chen, Andrew I., Chen, H., Choumilov, Evgueni, Choutko, Vitali, Egorov, Alexander, Eline, Alexandre, Eppling, Frederic J., Fisher, Peter H., Galaktionov, Y., Goglov, Pavel, Heil, Melanie, Hsieh, Tsai-hsiu, Kounina, Olga, Kounine, Andrei, Koutsenko, Vladimir, Krafczyk, Matthew Scott, Lebedev, Alexei, Li, J. Q., Li, Q., Plyaskin, Vasily, Rozhkov, Andrey B., Shi, X. Y., Sun, Wei, Sun, W. H., Ting, Samuel, Ting, Susan Marks, Vaurynovich, Siarhei S., Wang, Xiaozhen, Weng, Zhili, Willenbrock, Manfred, Xie, M., Xu, Weiwei, Yan, Q., Zhang, S. D., Zuccon, Paolo, Azzarello, Philipp, Bourquin, Maurice, Cadoux, Franck, Cortina Gil, Eduardo, Haas, Daniel, Habiby Alaoui, Marion, Leluc, Catherine, Li, Yang, Paniccia, Mercedes, Pohl, Martin, Rapin, Divic Jean, Saouter, Pierre, Vitillo, Stefania, Wu, Xin, Aguilar, M, Aisa, D, Alpat, B, Alvino, A, Ambrosi, G, Andeen, K, Arruda, L, Attig, N, Azzarello, P, Bachlechner, A, Barao, F, Barrau, A, Barrin, L, Bartoloni, A, Basara, L, Battarbee, M, Battiston, R, Bazo, J, Becker, U, Behlmann, M, Beischer, B, Berdugo, J, Bertucci, B, Bindi, V, Bizzaglia, S, Bizzarri, M, Boella, G, de Boer, W, Bollweg, K, Bonnivard, V, Borgia, B, Borsini, S, Boschini, M, Bourquin, M, Burger, J, Cadoux, F, Cai, X, Capell, M, Caroff, S, Casaus, J, Castellini, G, Cernuda, I, Cerreta, D, Cervelli, F, Chae, M, Chang, Y, Chen, A, Chen, G, Chen, H, Cheng, L, Chou, H, Choumilov, E, Choutko, V, Chung, C, Clark, C, Clavero, R, Coignet, G, Consolandi, C, Contin, A, Corti, C, Gil, E, Coste, B, Creus, W, Crispoltoni, M, Cui, Z, Dai, Y, Delgado, C, Della Torre, S, Demirköz, M, Derome, L, Di Falco, S, Di Masso, L, Dimiccoli, F, Díaz, C, von Doetinchem, P, Donnini, F, Duranti, M, D’Urso, D, Egorov, A, Eline, A, Eppling, F, Eronen, T, Fan, Y, Farnesini, L, Feng, J, Fiandrini, E, Fiasson, A, Finch, E, Fisher, P, Formato, V, Galaktionov, Y, Gallucci, G, García, B, García López, R, Gargiulo, C, Gast, H, Gebauer, I, Gervasi, M, Ghelfi, A, Giovacchini, F, Goglov, P, Gong, J, Goy, C, Grabski, V, Grandi, D, Graziani, M, Guandalini, C, Guerri, I, Guo, K, Haas, D, Habiby, M, Haino, S, Han, K, He, Z, Heil, M, Hoffman, J, Hsieh, T, Huang, Z, Huh, C, Incagli, M, Ionica, M, Jang, W, Jinchi, H, Kanishev, K, Kim, G, Kim, K, Kirn, T, Korkmaz, M, Kossakowski, R, Kounina, O, Kounine, A, Koutsenko, V, Krafczyk, M, LA VACCA, G, Laudi, E, Laurenti, G, Lazzizzera, I, Lebedev, A, Lee, H, Lee, S, Leluc, C, Li, H, Li, J, Li, Q, Li, T, Li, W, Li, Y, Li, Z, Lim, S, Lin, C, Lipari, P, Lippert, T, Liu, D, Liu, H, Lolli, M, Lomtadze, T, Lu, M, Lu, S, Lu, Y, Luebelsmeyer, K, Luo, F, Luo, J, Lv, S, Majka, R, Mañá, C, Marín, J, Martin, T, Martínez, G, Masi, N, Maurin, D, Menchaca Rocha, A, Meng, Q, Mo, D, Morescalchi, L, Mott, P, Müller, M, Nelson, T, Ni, J, Nikonov, N, Nozzoli, F, Nunes, P, Obermeier, A, Oliva, A, Orcinha, M, Palmonari, F, Palomares, C, Paniccia, M, Papi, A, Pauluzzi, M, Pedreschi, E, Pensotti, S, Pereira, R, Picot Clemente, N, Pilo, F, Piluso, A, Pizzolotto, C, Plyaskin, V, Pohl, M, Poireau, V, Putze, A, Quadrani, L, Qi, X, Qin, X, Qu, Z, Räihä, T, Rancoita, P, Rapin, D, Ricol, J, Rodríguez, I, Rosier Lees, S, Rozhkov, A, Rozza, D, Sagdeev, R, Sandweiss, J, Saouter, P, Schael, S, Schmidt, S, von Dratzig, A, Schwering, G, Scolieri, G, Seo, E, Shan, B, Shan, Y, Shi, J, Shi, X, Shi, Y, Siedenburg, T, Son, D, Song, J, Spada, F, Spinella, F, Sun, W, Tacconi, M, Tang, C, Tang, X, Tang, Z, Tao, L, Tescaro, D, Ting, S, Tomassetti, N, Torsti, J, Türkoğlu, C, Urban, T, Vagelli, V, Valente, E, Vannini, C, Valtonen, E, Vaurynovich, S, Vecchi, M, Velasco, M, Vialle, J, Vitale, V, Vitillo, S, Wang, L, Wang, N, Wang, Q, Wang, R, Wang, X, Wang, Z, Weng, Z, Whitman, K, Wienkenhöver, J, Willenbrock, M, Wu, H, Wu, X, Xia, X, Xie, M, Xie, S, Xiong, R, Xu, N, Xu, W, Yan, Q, Yang, J, Yang, M, Yang, Y, Ye, Q, Yi, H, Yu, Y, Yu, Z, Zeissler, S, Zhang, C, Zhang, J, Zhang, M, Zhang, S, Zhang, X, Zhang, Z, Zheng, Z, Zhuang, H, Zhukov, V, Zichichi, A, Zimmermann, N, Zuccon, P, Aguilar, M., Aisa, D., Alpat, B., Alvino, A., Ambrosi, G., Andeen, K., Arruda, L., Attig, N., Azzarello, P., Bachlechner, A., Barao, F., Barrau, A., Barrin, L., Bartoloni, A., Basara, L., Battarbee, M., Battiston, R., Bazo, J., Becker, U., Behlmann, M., Beischer, B., Berdugo, J., Bertucci, B., Bindi, V., Bizzaglia, S., Bizzarri, M., Boella, G., de Boer, W., Bollweg, K., Bonnivard, V., Borgia, B., Borsini, S., Boschini, M. j., Bourquin, M., Burger, J., Cadoux, F., Cai, X. d., Capell, M., Caroff, S., Casaus, J., Castellini, G., Cernuda, I., Cerreta, D., Cervelli, F., Chae, M. j., Chang, Y. h., Chen, A. i., Chen, G. m., Chen, H. s., Cheng, L., Chou, H. y., Choumilov, E., Choutko, V., Chung, C. h., Clark, C., Clavero, R., Coignet, G., Consolandi, C., Contin, A., Corti, C., Gil, E. Cortina, Coste, B., Creus, W., Crispoltoni, M., Cui, Z., Dai, Y. m., Delgado, C., Della Torre, S., Demirköz, M. b., Derome, L., Di Falco, S., Di Masso, L., Dimiccoli, F., Díaz, C., von Doetinchem, P., Donnini, F., Duranti, M., D’Urso, D., Egorov, A., Eline, A., Eppling, F. j., Eronen, T., Fan, Y. y., Farnesini, L., Feng, J., Fiandrini, E., Fiasson, A., Finch, E., Fisher, P., Formato, V., Gallucci, G., García, B., García-López, R., Gargiulo, C., Gast, H., Gebauer, I., Gervasi, M., Ghelfi, A., Giovacchini, F., Goglov, P., Gong, J., Goy, C., Grabski, V., Grandi, D., Graziani, M., Guandalini, C., Guerri, I., Guo, K. h., Haas, D., Habiby, M., Haino, S., Han, K. c., He, Z. h., Heil, M., Hoffman, J., Hsieh, T. h., Huang, Z. c., Huh, C., Incagli, M., Ionica, M., Jang, W. y., Jinchi, H., Kanishev, K., Kim, G. n., Kim, K. s., Kirn, Th., Korkmaz, M. a., Kossakowski, R., Kounina, O., Kounine, A., Koutsenko, V., Krafczyk, M. s., La Vacca, G., Laudi, E., Laurenti, G., Lazzizzera, I., Lebedev, A., Lee, H. t., Lee, S. c., Leluc, C., Li, H. l., Li, J. q., Li, T. x., Li, W., Li, Y., Li, Z. h., Li, Z. y., Lim, S., Lin, C. h., Lipari, P., Lippert, T., Liu, D., Liu, H., Liu, Hu, Lolli, M., Lomtadze, T., Lu, M. j., Lu, S. q., Lu, Y. s., Luebelsmeyer, K., Luo, F., Luo, J. z., Lv, S. s., Majka, R., Mañá, C., Marín, J., Martin, T., Martínez, G., Masi, N., Maurin, D., Menchaca-Rocha, A., Meng, Q., Mo, D. c., Morescalchi, L., Mott, P., Müller, M., Nelson, T., Ni, J. q., Nikonov, N., Nozzoli, F., Nunes, P., Obermeier, A., Oliva, A., Orcinha, M., Palmonari, F., Palomares, C., Paniccia, M., Papi, A., Pauluzzi, M., Pedreschi, E., Pensotti, S., Pereira, R., Picot-Clemente, N., Pilo, F., Piluso, A., Pizzolotto, C., Plyaskin, V., Pohl, M., Poireau, V., Putze, A., Quadrani, L., Qi, X. m., Qin, X., Qu, Z. y., Räihä, T., Rancoita, P. g., Rapin, D., Ricol, J. s., Rodríguez, I., Rosier-Lees, S., Rozhkov, A., Rozza, D., Sagdeev, R., Sandweiss, J., Saouter, P., Schael, S., Schmidt, S. m., von Dratzig, A. Schulz, Schwering, G., Scolieri, G., Seo, E. s., Shan, B. s., Shan, Y. h., Shi, J. y., Shi, X. y., Shi, Y. m., Siedenburg, T., Son, D., Song, J. w., Spada, F., Spinella, F., Sun, W., Sun, W. h., Tacconi, M., Tang, C. p., Tang, X. w., Tang, Z. c., Tao, L., Tescaro, D., Ting, Samuel C. C., Ting, S. m., Tomassetti, N., Torsti, J., Türkoğlu, C., Urban, T., Vagelli, V., Valente, E., Vannini, C., Valtonen, E., Vaurynovich, S., Vecchi, M., Velasco, M., Vialle, J. p., Vitale, V., Vitillo, S., Wang, L. q., Wang, N. h., Wang, Q. l., Wang, R. s., Wang, X., Wang, Z. x., Weng, Z. l., Whitman, K., Wienkenhöver, J., Willenbrock, M., Wu, H., Wu, X., Xia, X., Xie, S., Xiong, R. q., Xu, N. s., Xu, W., Yang, J., Yang, M., Yang, Y., Ye, Q. h., Yi, H., Yu, Y. j., Yu, Z. q., Zeissler, S., Zhang, C., Zhang, J. h., Zhang, M. t., Zhang, S. d., Zhang, S. w., Zhang, X. b., Zhang, Z., Zheng, Z. m., Zhuang, H. l., Zhukov, V., Zichichi, A., Zimmermann, N., Zuccon, P., UCL - SST/IRMP - Institut de recherche en mathématique et physique, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-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), and AMS Collaboration
- Subjects
Astrophysics and Astronomy ,Astrophysics::High Energy Astrophysical Phenomena ,General Physics and Astronomy ,chemistry.chemical_element ,Cosmic ray ,Astrophysics ,ddc:500.2 ,Power law ,Helium ,Space missions ,[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,FIS/05 - ASTRONOMIA E ASTROFISICA ,Physics and Astronomy (all) ,Rigidity (electromagnetism) ,International Space Station ,Alpha Magnetic Spectrometer ,ddc:550 ,AMS ,Helium Flux, Primary Cosmic Rays ,Cosmic rays ,Physics ,Spectral index ,ta114 ,Cosmic Rays, Cosmic Helium ,Spectral density ,ASTROFÍSICA ,Computational physics ,FIS/01 - FISICA SPERIMENTALE ,chemistry ,Cosmic ray measurement ,Cosmology ,Rigidity ,Space stations ,Spectrometers - Abstract
Physical review letters 115(21), 211101 (2015). doi:10.1103/PhysRevLett.115.211101, Published by APS, College Park, Md.
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- 2015
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43. Propagation of Solar Energetic Particles during Multiple Coronal Mass Ejection Events
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Firas Al-Hamadani, Silja Pohjolainen, and Eino Valtonen
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Physics ,education.field_of_study ,010504 meteorology & atmospheric sciences ,Shock (fluid dynamics) ,Solar energetic particles ,Population ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Electron ,01 natural sciences ,Particle acceleration ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,0103 physical sciences ,Coronal mass ejection ,education ,Interplanetary spaceflight ,010303 astronomy & astrophysics ,Event (particle physics) ,Solar and Stellar Astrophysics (astro-ph.SR) ,0105 earth and related environmental sciences - Abstract
We study solar energetic particle (SEP) events during multiple solar eruptions. The analysed sequences, on 24-26 November 2000, 9-13 April 2001, and 22-25 August 2005, consisted of halo-type coronal mass ejections (CMEs) that originated from the same active region and were associated with intense flares, EUV waves, and interplanetary (IP) radio type II and type III bursts. The first two solar events in each of these sequences showed SEP enhancements near Earth, but the third in the row did not. We observed that in these latter events the type III radio bursts were stopped at much higher frequencies than in the earlier events, indicating that the bursts did not reach the typical plasma density levels near Earth. To explain the missing third SEP event in each sequence, we suggest that the earlier-launched CMEs and the CME-driven shocks either reduced the seed particle population and thus led to inefficient particle acceleration, or that the earlier-launched CMEs and shocks changed the propagation paths or prevented the propagation of both the electron beams and SEPs, so that they did not get detected near Earth even when the shock arrivals were recorded., Comment: Solar Physics, accepted (Dec. 2015)
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- 2015
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44. Investigating the Origins of Two Extreme Solar Particle Events: Proton Source Profile and Associated Electromagnetic Emissions
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Jeongwoo Lee, Rok-Soon Kim, M. J. Reiner, Victor J. Pizzo, Kyung-Suk Cho, Leon Kocharov, Ilya Usoskin, Leonid Didkovsky, Rami Vainio, Silja Pohjolainen, Marian Karlicky, Dale E. Gary, Alexander Mishev, Timo Laitinen, Andreas Klassen, and Eino Valtonen
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010504 meteorology & atmospheric sciences ,Astrophysics::High Energy Astrophysical Phenomena ,Interplanetary medium ,Magnetosphere ,F500 ,Astrophysics ,01 natural sciences ,7. Clean energy ,law.invention ,law ,0103 physical sciences ,Coronal mass ejection ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences ,Physics ,Solar observatory ,Astronomy ,Astronomy and Astrophysics ,Solar wind ,13. Climate action ,Space and Planetary Science ,Physics::Space Physics ,Solar particle event ,Event (particle physics) ,Flare - Abstract
We analyze the high-energy particle emission from the Sun in two extreme solar particle events, in which protons are accelerated to relativistic energies and can cause a significant signal even in the ground-based particle detectors. Analysis of a relativistic proton event is based on modeling of the particle transport and interaction, from a near-Sun source through the solar wind and the Earth’s magnetosphere and atmosphere to a detector on the ground. This allows us to deduce the time profile of the proton source at the Sun and compare it with observed electromagnetic emissions. The 2 May 1998 event is associated with flare and coronal mass ejection (CME) well observed by the Nan¸cay Radioheliograph, so that the images of radio sources are available. For the 2 November 2003 event, there are available the low-corona images of the CME liftoff obtained at the Mauna Loa Solar Observatory. Those complementary data sets are analyzed jointly with the broadband dynamic radio spectra, EUV images and other data available for both events. We find a common scenario for both eruptions, including the flare’s dual impulsive phase, the CME-launch-associated decimetric-continuum burst, and the late, low-frequency type III radio bursts at the time of the relativistic proton injection into the interplanetary medium. The analysis supports the idea that the two considered events start with emission of relativistic protons previously accelerated during the flare and CME launch, then trapped in large-scale magnetic loops and later released by the expanding CME.
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- 2017
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45. Precision Measurement of the(e++e−)Flux in Primary Cosmic Rays from 0.5 GeV to 1 TeV with the Alpha Magnetic Spectrometer on the International Space Station
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Y. Y. Fan, Massimo Gervasi, A. Fiasson, Roberto Battiston, N. Masi, F. Luo, L. Tao, L. Barrin, M. Capell, M. Paniccia, A. Schulz von Dratzig, M. Pohl, B. Borgia, C. Leluc, G. Gallucci, S. S. Vaurynovich, Julio C. Marín, Miaoran Lu, Yongyao Li, G. Boella, K. C. Han, J. Z. Luo, F. Giovacchini, Yun Shi, Q. L. Wang, Luca Morescalchi, Lucio Quadrani, Samuel C.C. Ting, Tim Martin, B. Beischer, V. Bonnivard, C. Delgado, G. Scolieri, Mingming Yang, M. Habiby, A. Malinin, Zhixiang Tang, C. P. Tang, D. C. Mo, A. Eline, J. Y. Shi, M. Müller, Maria Ionica, G. Schwering, J. S. Ricol, Lin Cheng, W. De Boer, K. H. Guo, Dong-Chul Son, S. Schael, X. W. Tang, P. Saouter, Teimuraz Lomtadze, M. Duranti, Yu. Galaktionov, R. J. García-López, N. Nikonov, Liqiu Wang, D. D'Urso, Elisa Laudi, J. Hoffman, I. Guerri, S. M. Schmidt, M. J. Chae, C. Guandalini, K. Luebelsmeyer, Y. J. Yu, H. T. Lee, J. Q. Ni, G. Martinez, C. Palomares, C. Clark, V. Poireau, H. Jinchi, D. Aisa, N. Attig, A. Alvino, J. P. Vialle, L. Basara, Z. M. Zheng, S. Kunz, J. Casaus, Z. Q. Yu, K. Bollweg, A.I. Oliva, A. Ghelfi, Valerio Vagelli, E. Choumilov, X. M. Qi, A. Piluso, D. Rozza, S. Borsini, I. Cernuda, G. Castellini, Jinglai Li, V. Choutko, G. Ambrosi, F. Cervelli, S. Lim, Bruna Bertucci, D. Grandi, T. Urban, R. Kossakowski, Carlos Díaz, S. Bizzaglia, M. J. Boschini, L. Di Masso, I. Gebauer, B. Coste, V. Cascioli, Fabrizio Giulio Luca Pilo, M. Orcinha, D. Tescaro, Timothy H. Hsieh, Manuela Vecchi, W. H. Sun, W. Y. Jang, P. Lipari, T. Räihä, M. Aguilar, Ruiguang Wang, C. Pizzolotto, M. Bizzarri, E. Fiandrini, Y. H. Shan, A. Bartoloni, G. N. Kim, Zhihua Zhang, C. Vannini, Haifeng Li, K. Kanishev, Nicola Tomassetti, H. L. Zhuang, L. Farnesini, M. Graziani, F. Spinella, X. Y. Shi, Z. L. Weng, Chia-Hui Lin, D. Rapin, H. S. Chen, V. Plyaskin, J. Yang, J. Gong, S. Xie, C. Goy, Behcet Alpat, E. Postaci, C. Sbarra, A. Barrau, G. M. Cheng, P. von Doetinchem, Roald Z. Sagdeev, X. D. Cai, Mauro Tacconi, G. Coignet, Antje Putze, Jianfeng Feng, B. S. Shan, Won Kyu Calvin Sun, Q. H. Ye, M. B. Demirköz, H. Yi, Wei Li, K. Whitman, H. Y. Chou, S. Della Torre, Q. Meng, R. D. Majka, F. Donnini, Changgi Huh, X. Xia, J. Wienkenhöver, Z. Cui, Hengchang Liu, E. Pedreschi, W. J. Du, Kwangsoo Kim, Andrei Kounine, Sadakazu Haino, Q. Yan, F. Spada, A. Papi, G. Bigongiari, S. Caroff, Bruce Rafael Mellado Garcia, Paolo Zuccon, Y. H. Chang, R. Clavero, N. Zimmermann, J. J. Torsti, S. Pensotti, Zhao Wang, Antonino Zichichi, Henning Gast, I. Rodríguez, J. Berdugo, Luísa Arruda, A. Rozhkov, S. Zeissler, A. Obermeier, S. Di Falco, Valery Zhukov, C. Consolandi, T. X. Li, Varlen Grabski, P. Mott, M. Incagli, M. Pauluzzi, J. D. Burger, T. Siedenburg, Claudio Corti, M. Bourquin, J. Bazo, R. Q. Xiong, Mayda Velasco, Corrado Gargiulo, P. Azzarello, Zhiqi Huang, S. C. Lee, S. S. Lv, J. Sandweiss, A. Chikanian, Z. Y. Li, A. Bachlechner, X. B. Zhang, Eun-Suk Seo, X. Q. Wang, Ying Lu, S. Rosier-Lees, V. Koutsenko, Eino Valtonen, Z. H. Li, Qiang Li, W. Gillard, C. H. Chung, G. La Vacca, David Maurin, Rui Miguel Faisca Rodrigues Pereira, M. T. Zhang, M. Crispoltoni, M. Behlmann, Laurent Derome, Ningsheng Xu, Franck Cadoux, P. Nunes, D. Liu, D. Schuckardt, Matthias Heil, G. Laurenti, A. I. Chen, P. Goglov, Alexandre Lebedev, P. G. Rancoita, M. S. Krafczyk, I. Lazzizzera, M. Xie, C. Mañá, Veronica Bindi, Z. H. He, F. Nozzoli, C. Zurbach, T. Eronen, W. Xu, T. Kirn, C. Türkoğlu, Arturo Alejandro Menchaca-Rocha, Gongming Xin, Markus Battarbee, E. Finch, J. H. Zhang, K. Andeen, F. Barao, U. Becker, Thomas Lippert, F. J. Eppling, P. H. Fisher, S. M. Ting, F. Palmonari, M. Dai, O. Kounina, H. Wu, Andrea Contin, F. Dimiccoli, and E. Valente
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Nuclear physics ,Physics ,Primary (astronomy) ,International Space Station ,Hardware_INTEGRATEDCIRCUITS ,Alpha Magnetic Spectrometer ,General Physics and Astronomy ,Flux ,Cosmic ray ,Hardware_PERFORMANCEANDRELIABILITY ,Hardware_REGISTER-TRANSFER-LEVELIMPLEMENTATION ,Hardware_LOGICDESIGN - Published
- 2014
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46. Release timescales of solar energetic particles in the low corona
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Karl-Ludwig Klein, M. Subirà, E. Talew, W. Dröge, Bernd Heber, Olga Malandraki, Rami Vainio, S. Braune, Blai Sanahuja, Neus Agueda, R. Rodríguez-Gasén, D. Heynderickx, Nicole Vilmer, Athanasios Papaioannou, Ilya Usoskin, Alexander Nindos, Eino Valtonen, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Demokritos University of Thrace, Department of Electrical Engineering, Dept. Astronomica i Meteorologia, Universitat de Barcelona (UB), Institut für Experimentelle und Angewandte Physik [Kiel] (IEAP), Christian-Albrechts-Universität zu Kiel (CAU), Sodankylä Geophysical Observatory, University of Oulu, Belgisch Instituut voor Ruimte-Aëronomie (BIRA), Space Research Laboratory [Turku] (SRL), Department of Physics and Astronomy [Turku], and University of Turku-University of Turku
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Physics ,[PHYS]Physics [physics] ,Solar flare ,Solar energetic particles ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,Astrophysics::High Energy Astrophysical Phenomena ,Interplanetary medium ,Astronomy ,Astronomy and Astrophysics ,Context (language use) ,Electron ,Astrophysics ,Radiation ,Corona ,13. Climate action ,Space and Planetary Science ,Physics::Space Physics ,Interplanetary spaceflight ,ComputingMilieux_MISCELLANEOUS - Abstract
Aims. We present a systematic study of the timing and duration of the release processes of near-relativistic (NR; >50 keV) electrons in the low corona.Methods. We analyze seven well-observed events using in situ measurements by both the ACE and Wind spacecraft and context electromagnetic observations in soft X-rays, radio, hard X-rays and white light. We make use of velocity dispersion analysis to estimate the release time of the first arriving electrons and compare with the results obtained by using a simulation-based approach, taking interplanetary transport effects into account to unfold the NR electron release time history from in situ measurements.Results. The NR electrons observed in interplanetary space appear to be released during either short ( 30 min) or long (> 2 h) periods. The observation of NR electron events showing beamed pitch-angle distributions (PADs) during several hours is the clearest observational signature of sustained release in the corona. On the other hand, the in situ observation of PADs isotropizing in less than a couple of hours is a clear signature of a prompt release of electrons in the low corona. Short release episodes appear to originate in solar flares, in coincidence with the timing of the observed type III radio bursts. Magnetic connectivity plays an important role. Only type III radio bursts reaching the local plasma line measured at 1 AU are found to be related with an associated release episode in the low corona. Other type III bursts may also have a release of NR electrons associated with them, but these electrons do not reach L1. Long release episodes appear associated with signatures of long acceleration processes in the low corona (long decay of the soft X-ray emission, type IV radio bursts, and time-extended microwave emission). Type II radio bursts are reported for most of the events and do not provide a clear discrimination between short and long release timescales.
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- 2014
- Full Text
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47. Electronics for the RADMON instrument on the Aalto-1 student satellite
- Author
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Risto Punkkinen, M. Maattanen, Hannu-Pekka Hedman, Rami Vainio, Tero Säntti, J. Pesonen, M. Lindroos, Arttu Punkkinen, Edward Hæggström, Eino Valtonen, A. Ilmanen, J. Peltonen, and J. Pentikainen
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Physics ,business.industry ,Electrical engineering ,Measure (physics) ,7. Clean energy ,Photodiode ,law.invention ,law ,Electronic engineering ,Silicon detector ,Radiation monitoring ,Satellite ,Electronics ,business ,Field-programmable gate array - Abstract
RADMON is a small, low cost and low power instrument developed for the Aalto-1 student satellite. RADMON will measure protons (10-200 MeV) and electrons (0.7-10 MeV) in low-Earth orbit using a silicon detector and a CsI-scintillator with photodiode readout. The instrument, the sensors and the electronics are described in this article. RADMON uses FPGA logic to analyze the continuously digitized sensor data at 10 MHz. We expect the instrument to be much faster than traditional radiation monitors with analog pulse storing. Fabrication of the electronics is now completed and the testing has been started. RADMON will be integrated into the Aalto-1 satellite in the summer of 2014. Educationally RADMON has been both rewarding and difficult: half a dozen master's theses have so far been completed within the project. On the other hand there have been significant delays and continuity problems in RADMON due to the changing workforce.
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- 2014
- Full Text
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48. Background reduction for quiet time particle fluxes aboard the Solar and Heliospheric Observatory
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J. J. Torsti, Reinhold Müller-Mellin, Karoly Kecskemety, Eino Valtonen, and H. Kunow
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Physics ,Solar minimum ,Atmospheric Science ,Ecology ,Solar energetic particles ,Proton ,Paleontology ,Soil Science ,Forestry ,Electron ,Astrophysics ,Aquatic Science ,Oceanography ,Relativistic particle ,Geophysics ,Space and Planetary Science ,Geochemistry and Petrology ,Observatory ,Physics::Space Physics ,Earth and Planetary Sciences (miscellaneous) ,Astrophysics::Solar and Stellar Astrophysics ,Particle ,Heliosphere ,Earth-Surface Processes ,Water Science and Technology - Abstract
Two versions of a method are presented to determine the background of energetic particle telescopes during low-flux periods at low energies. Traditional procedures first evaluate pulse heights of particle sensors working in coincidence then select certain areas of the ΔE/Δx versus E plane, where E is energy, and finally, accept all events falling on those areas as real particles. Such methods, however, often fail during low-flux conditions, as the background may become comparable to the genuine particle flux. The alternative methods suggested here analyze the shape of the distribution near the track of genuine particles and provide statistical estimation of its parameters to separate the background from the real particle flux. Results are presented for protons and helium during quiet activity periods of the recent solar minimum using data from energetic particle telescopes Energetic and Relativistic Nuclei and Electron (ERNE) Low Energy Detector (LED) and Comprehensive Suprathermal and Energetic Particle Analyzer (COSTEP) Electron Proton Helium Instrument (EPHIN) aboard the Solar and Heliospheric Observatory (SOHO) spacecraft. SOHO is a project of international collaboration between the European Space Agency and NASA.
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- 2001
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49. SEPs and CMEs during cycle 23
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Pertti Makela, Nat Gopalswamy, Sachiko Akiyama, Hong Xie, Seiji Yashiro, and Eino Valtonen
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Physics ,Space and Planetary Science ,Coronal cloud ,Astronomy ,Astronomy and Astrophysics - Abstract
We present a study of solar energetic particles (SEPs) in association with coronal mass ejections (CMEs) and type II radio bursts. The particle and CME observations cover the years 1996–2007. We find that heavy-ion events in association with type II bursts and proton events are produced in more western and most energetic CMEs. In addition, the source distribution of type II associated proton events with heavy ions reminds the source distribution expected for events with flare particles. Therefore, the estimation of relative contributions by flares and shocks in SEP events and separation of suggested different particle acceleration models is complicated.
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- 2008
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50. Observations of galactic cosmic ray modulation during Earth-directed coronal mass ejections
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Pertti Makela, M. Teittinen, Eino Valtonen, E. Riihonen, F. M. Ipavich, and J. J. Torsti
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Physics ,Range (particle radiation) ,Proton ,chemistry.chemical_element ,Astronomy ,Flux ,Cosmic ray ,Astrophysics ,Geophysics ,chemistry ,Coronal mass ejection ,General Earth and Planetary Sciences ,Ejecta ,Interplanetary spaceflight ,Helium - Abstract
We describe three cosmic-ray decreases observed by the energetic particle telescope ERNE on board SOHO spacecraft during the period January–May, 1997. The decreases in cosmic-ray proton intensities in the energy range above 50 MeV were observed after the passage of interplanetary shocks on February 9, April 10, and May 15. All the shocks were produced by Earth-directed coronal mass ejections. The amplitudes of the decreases compared to the counting rates just before the shock arrival were 8.5%, 14%, and 7%, respectively. The observed recovery times were 1, 4.2, and 5 days, respectively. After the February and May events the pre-shock levels were reached, but in the April event the recovery was only to 3% below this level. In each case, there were also clear indications of the passage of the ejecta. The energy dependences of the cosmic-ray helium flux decreases at 12–100 MeV/n were similar to each other in the April and May events, while in the February event the decrease was less pronounced.
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- 1998
- Full Text
- View/download PDF
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