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9 results on '"SOLAR WIND [SUN]"'

1. The source of unusual coronal upflows with photospheric abundance in a solar active region

Author

Harra, Louise, Mandrini, Cristina, Brooks, David, Barczynski, Krzysztof, Mac Cormack, Cecilia, Cristiani, Germán, Mandal, Sudip, Sterling, Alphonse C., Martinez Pillet, Valentin, Janitzek, Nils, Schühle, Udo, Berghmans, David, Auchère, Frédéric, Aznar Cuadrado, Regina, Buchlin, Éric, Kraaikamp, Emil, Long, David, Parenti, Susanna, Peter, Hardi, Rodriguez, Luciano, Smith, Phil, Teriaca, Luca, Verbeeck, Cis, and Zhukov, Andrei N.

Subjects
Sun: general, sunspots, solar wind, general, solar wind [Sun]
Abstract

Context. Upflows in the corona are of importance, as they may contribute to the solar wind. There has been considerable interest in upflows from active regions (ARs). The coronal upflows that are seen at the edges of active regions have coronal elemental composition and can contribute to the slow solar wind. The sources of the upflows have been challenging to determine because they may be multiple, and the spatial resolution of previous observations is not yet high enough. Aims. In this article, we analyse coronal upflows in AR 12960 that are unusually close to the sunspot umbra. We analyse their properties, and we attempt to determine if it is possible that they feed into the slow solar wind. Methods. We analysed the activity in the upflow region in detail using a combination of Solar Orbiter EUV images at high spatial and temporal resolution, Hinode/EUV Imaging Spectrometer data, and observations from instruments on board the Solar Dynamics Observatory. This combined dataset was acquired during the first Solar Orbiter perihelion of the science phase, which provided a spatial resolution of 356 km for two pixels. Doppler velocity, density, and plasma composition determinations, as well as coronal magnetic field modelling, were carried out to understand the source of the upflows. Results. We observed small magnetic fragments, called moving magnetic features (MMFs), moving away from the sunspot in the active region. Specifically, they moved towards the sunspot from the edge of the penumbra where a small positive polarity connects to the umbra via small-scale and very dynamic coronal loops. At this location, small dark grains are evident and flow along penumbral filaments in continuum images. The magnetic field modelling showed small low-lying loops anchored close to the umbral magnetic field. The high-resolution data of the Solar Orbiter EUV Imagers showed the dynamics of these small loops, which last on time scales of only minutes. The edges of these small loops are the location of the coronal upflow that has photospheric abundance., Astronomy & Astrophysics, 675, ISSN:0004-6361, ISSN:1432-0746

Published
2023

2. Structure of the photospheric magnetic field during sector crossings of the heliospheric magnetic field

Author

Tibebu Getachew, Ilpo Virtanen, and Kalevi Mursula

Subjects
Physics, Photosphere, Solar observatory, heliosphere [Sun], 010504 meteorology & atmospheric sciences, photosphere [Sun], Northern Hemisphere, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, solar wind [Sun], L-shell, Solar cycle, Solar wind, Nuclear magnetic resonance, magnetic fields [Sun], Space and Planetary Science, 0103 physical sciences, activity [Sun], Interplanetary magnetic field, Mercury's magnetic field, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

The photospheric magnetic field is the source of the coronal and heliospheric magnetic fields (HMF), but their mutual correspondence is non-trivial and depends on the phase of the solar cycle. The photospheric field during the HMF sector crossings observed at 1 AU has been found to contain enhanced field intensities and definite polarity ordering, forming regions called Hale boundaries. Here we separately study the structure of the photospheric field during the HMF sector crossings during Solar Cycles 21 – 24 for the four phases of each solar cycle. We use a refined version of Svalgaard’s list of major HMF sector crossings, mapped to the Sun using the solar wind speed observed at Earth, and the daily level-3 magnetograms of the photospheric field measured at the Wilcox Solar Observatory in 1976 – 2016. We find that the structure of the photospheric field corresponding to the HMF sector crossings and the existence and properties of the corresponding Hale bipolar regions varies significantly with solar cycle, solar cycle phase, and hemisphere. The Hale boundaries in more than half of the ascending, maximum, and declining phases are clear and statistically significant. The clearest Hale boundaries are found during the (+,−) HMF crossings in the northern hemisphere of odd Cycles 21 and 23, but less systematical during the (+,−) crossings in the southern hemisphere of even Cycles 22 and 24. No similar difference between odd and even cycles is found for the (−,+) crossings. This shows that the northern hemisphere has a more organized Hale pattern overall. The photospheric field distribution also depicts a larger area for the field of the northern hemisphere during the declining and minimum phases, in a good agreement with the bashful ballerina phenomenon.

Published
2017

3. Folding ion rays in comet C/2004 Q2 (Machholz) and the connection with the solar wind

Author

Maarten Reyniers, Pieter Degroote, Dennis Bodewits, Research unit Astroparticle Physics, and KVI - Center for Advanced Radiation Technology

Subjects
Ccd camera, Comet, FOS: Physical sciences, disconnection, Astrophysics, general [comets], Ion, law.invention, comets : individual : C/ 2004 Q2 (Machholz), Telescope, tail, Observational evidence, charge, law, gas, emission, HALLEY, Physics, TAIL, individual : c/ 2004 q2 (machholz) [comets], comets : general, Astrophysics (astro-ph), Astronomy and Astrophysics, DISCONNECTION, halley, Folding (chemistry), Solar wind, Space and Planetary Science, GAS, Satellite, EMISSION, CHARGE, solar wind [sun], Sun : solar wind
Abstract

The appearance of folding ion rays in cometary comae is still not very well understood, so our aim is to gain more insight into the role of the local solar wind in the formation of these structures. Comet C/2004 Q2 (Machholz) was intensively monitored during its closest approach to Earth (January 2005) with the CCD camera Merope mounted on the Flemish 1.2m Mercator telescope, in three different bands (Geneva U and B and Cousins I). Spectacular ion rays, thin ionic structures rapidly folding tailward, were recorded in the U band during one night, January 12th. Data from the SOHO satellite that was extrapolated corotationally to the position of the comet showed that the ion rays were formed during a sudden change in the in-situ solar wind state. We were able to succesfully correlate a high-speed solar wind stream with the appearance of folding ion rays. To our knowledge, this is the first clear observational evidence that folding ion rays in cometary comae are produced by a sudden change in the local solar wind state., Comment: 4 pages, 4 figures, accepted by A&A

Published
2008

4. The Solar Minimum Corona from Differential Emission Measure Tomography

Author

Vasquez, Alberto Marcos, Frazin, Richard A., and Manchester IV, Ward B.

Subjects
Astronomía, corona [Sun], magnetic fields [Sun], Ciencias Físicas, activity [Sun], solar wind [Sun], CIENCIAS NATURALES Y EXACTAS
Abstract

We present results derived from a dual-spacecraft tomographic reconstruction of the solar corona’s three-dimensional (3D) extreme ultraviolet (EUV) emissivity. We use simultaneously taken STEREO A and B spacecraft EUVI images from Carrington rotation 2077 (2008, November 20 06:56 UT through December 17 14:34 UT). During this period, the spacecraft view-angles were separated by an average 85.4◦ which allowed for the reconstruction to be performed with data gathered in about 3/4 of a full solar rotational time. The EUV reconstructions provide the 3D emissivity in each of the three EUVI Fe bands, in the range of heights 1.00 to 1.25 Rs . We use this information to perform local differential emission measure (LDEM) analysis. Taking moments of the so-derived LDEM distributions gives the 3D values of the electron density, temperature and temperature spread. We determine relationships between the moments of the LDEM and the coronal magnetic field by making longitudinal averages of the moments, and relating them to the global-scale structures of a potential field source surface (PFSS) magnetic field model. In this way, we determine how the electron density, mean temperature, and temperature spread vary for different coronal structures. We draw conclusions about the relationship between the LDEM moments and the sources of the fast and slow solar winds, and the transition between the two regimes. Fil: Vasquez, Alberto Marcos. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: Frazin, Richard A.. University of Michigan; Estados Unidos Fil: Manchester IV, Ward B.. University of Michigan; Estados Unidos

Published
2010

5. Characteristics of magnetised plasma flow around stationary and expanding magnetic clouds

Author

Giorgi Dalakishvili, E. P. Romashets, Stefaan Poedts, and Horst Fichtner

Subjects
Physics, 1 au, Astronomy and Astrophysics, Astrophysics, Dipole model of the Earth's magnetic field, magnetic fields, plasmas, L-shell, bow-shock flows, Solar wind, Space and Planetary Science, Physics::Space Physics, evolution, Magnetic cloud, Magnetohydrodynamics, Interplanetary magnetic field, flux ropes, Mercury's magnetic field, magnetohydrodynamics (mhd), magnetohydrodynamics, solar wind [sun], Magnetosphere particle motion, fields, coronal mass ejections
Abstract

Aims: Studies of interplanetary magnetic clouds have shown that the characteristics of the region ahead of these objects, which are moving away from the Sun in the solar wind, play a role in determining their geo-efficiency, i.e. the kind and the degree of their effects on the Earth environment. Therefore, our main goal is to model and study the plasma parameters in the vicinity of interplanetary magnetic clouds. Methods: To this end we present a model in which the magnetic clouds are immersed in a magnetised plasma flow with a homogeneous magnetic field. We first calculate the resulting distortion of the external magnetic field and then determine the plasma velocity by employing the frozen-in condition. Results: Subsequently, the plasma density and pressure are expressed as functions of the magnetic field and the velocity field. Conclusions: The plasma flow parameters are determined by solving the time-independent ideal MHD equations for both the stationary regime and for the case of an expanding cylindrical magnetic cloud, thus extending previous results that appeared in the literature. ispartof: Astronomy & astrophysics vol:507 issue:2 pages:611-616 status: published

Published
2009

6. Outflows at the edges of active regions: Contribution to solar wind formation?

Author

Taro Sakao, Hirohisa Hara, Peter R. Young, L. van Driel-Gesztelyi, Cristina Hemilse Mandrini, D. N. Baker, Shinsuke Imada, Louise K. Harra, 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), Physique solaire, and 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, Ciencias Físicas, Flow (psychology), Imaging spectrometer, Astronomy, Astronomy and Astrophysics, X-ray telescope, SOLAR WIND [SUN], law.invention, Magnetic field, Telescope, Astronomía, Transverse plane, Solar wind, solar wind, Space and Planetary Science, law, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Outflow, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], SUN, MAGNETIC FIELDS, CIENCIAS NATURALES Y EXACTAS
Abstract

The formation of the slow solar wind has been debated for many years. In this Letter we show evidence of persistent outflow at the edges of an active region as measured by the EUV Imaging Spectrometer on board Hinode. The Doppler velocity ranged between 20 and 50 km s^-1 and was consistent with a steady flow seen in the X-Ray Telescope. The latter showed steady, pulsing outflowing material and some transverse motions of theloops. We analyze the magnetic field around the active region and produce a coronal magnetic field model. We determine from the latter that the outflow speeds adjusted for line-of-sight effects can reach over 100 km s^-1. We can interpret this outflow as expansion of loops that lie over the active region, which may either reconnect with neighboring large-scale loops or are likely to open to the interplanetary space. This material constitutes atleast part of the slow solar wind. Fil: Harra, L. K.. Mullard Space Science Laboratory; Reino Unido Fil: Sakao, T.. Institute of Space and Astronautical Science; Japón Fil: Mandrini, Cristina Hemilse. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: Hara, H.. National Astronomical Observatory of Japan; Japón Fil: Imada, S.. National Astronomical Observatory of Japan; Japón Fil: Young, P. R.. Rutherford Appleton Laboratory; Reino Unido Fil: van Driel Gesztelyi, Lidia. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Baker, D.. Mullard Space Science Laboratory; Reino Unido

Published
2008

7. Erratum: 'Outflows at the edges of active regions: Contribution to solar wind formation?'

Author

Harra, L. K., Sakao, T., Mandrini, Cristina Hemilse, Hara, H., Imada, S., Young, P.R., van Driel Gesztelyi, Lidia, and Baker, D.

Subjects
Astronomía, Ciencias Físicas, SOLAR WIND [SUN], MAGNETIC FIELDS [SUN], CIENCIAS NATURALES Y EXACTAS
Abstract

Fil: Harra, L. K.. Mullard Space Science Laboratory; Reino Unido Fil: Sakao, T.. Institute of Space and Astronautical Science; Japón Fil: Mandrini, Cristina Hemilse. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: Hara, H.. National Astronomical Observatory of Japan; Japón Fil: Imada, S.. National Astronomical Observatory of Japan; Japón Fil: Young, P.R.. Rutherford Appleton Laboratory; Reino Unido Fil: van Driel Gesztelyi, Lidia. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Baker, D.. Mullard Space Science Laboratory; Reino Unido

Published
2008

8. Study of the solar anisotropy of cosmic ray primaries of about 200 GeV energy with the L3+C muon detector

Author

Achard, P, Adriani, O, Aguilar-Benitez, M, van den Akker, M, Alcaraz, J, Alemanni, G, Allaby, J, Aloisio, A, Alviggi, M G, Anderhub, H, Andreev, Valery P, Anselmo, F, Arefev, A, Azemoon, T, Aziz, T, Bagnaia, P, Bajo, A, Baksay, G, Baksay, L, Bahr, J, Baldew, S V, Banerjee, S, Banerjee, Sw, Barczyk, A, Barillere, R, Bartalini, P, Basile, M, Batalova, N, Battiston, R, Bay, A, Becattini, F, Becker, U, Behner, F, Bellucci, L, Berbeco, R, Berdugo, J, Berges, P, Bertucci, B, Betev, B L, Biasini, M, Biglietti, M, Biland, A, Blaising, J J, Blyth, S C, Bobbink, G J, Bohm, A, Boldizsar, L, Borgia, B, Bottai, S, Bourilkov, D, Bourquin, M, Braccini, S, Branson, J G, Brochu, F, Burger, J D, Burger, W J, Cai, X D, Capell, M, Cara Romeo, G, Carlino, G, Cartacci, A, Casaus, J, Cavallari, F, Cavallo, N, Cecchi, C, Cerrada, M, Chamizo, M, Chiarusi, T, Chang, Y H, Chemarin, M, Chen, A, Chen, G, Chen, G M, Chen, H F, Chen, H S, Chiefari, G, Cifarelli, L, Cindolo, F, Clare, I, Clare, R, Coignet, G, Colino, N, Costantini, S, de la Cruz, B, Cucciarelli, S, van Dalen, J, de Asmundis, R, Deglon, P, Debreczeni, J, Degre, A, Dehmelt, K, Deiters, K, della Volpe, D, Delmeire, E, Denes, P, DeNotaristefani, F, De Salvo, A, Diemoz, M, Dierckxsens, M, Ding, L K, Dionisi, C, Dittmar, M, Doria, A, Dova, M T, Duchesneau, D, Duda, M, Duran, I, Echenard, B, Eline, A, El Hage, A, El Mamouni, H, Engler, A, Eppling, F J, Extermann, P, Faber, G, Falagan, M A, Falciano, S, Favara, A, Fay, J, Fedin, O, Felcini, M, Ferguson, T, Fesefeldt, H, Fiandrini, E, Field, J H, Filthaut, F, Fisher, W, Fisk, I, Forconi, G, Freudenreich, K, Furetta, C, Galaktionov, Iouri, Ganguli, S N, Garcia-Abia, Pablo, Gataullin, M, Gentile, S, Giagu, S, Gong, Z F, Grabosch, H J, Grenier, G, Grimm, O, Groenstege, H, Gruenewald, M W, Guida, M, Guo, Y N, Gupta, S, Gupta, V K, Gurtu, A, Gutay, L J, Haas, D, Haller, Ch, Hatzifotiadou, D, Hayashi, Y, He, Z X, Hebbeker, T, Herve, Alain, Hirschfelder, J, Hofer, H, Hohlmann, M, Holzner, G, Hou, S R, Huo, A X, Hu, Y, Ito, N, Jin, B N, Jing, C L, Jones, Lawrence W, de Jong, P, Josa-Mutuberria, I, Kantserov, V, Kaur, M, Kawakami, S, Kienzle-Focacci, M N, Kim, J K, Kirkby, Jasper, Kittel, W, Klimentov, A, Konig, A C, Kok, E, Korn, A, Kopal, M, Koutsenko, V, Kraber, M, Kuang, H H, Kraemer, R W, Kruger, A, Kuijpers, J, Kunin, A, Ladron de Guevara, P, Laktineh, I, Landi, G, Lebeau, M, Lebedev, A, Lebrun, P, Lecomte, P, Lecoq, P, Le Coultre, P, Le Goff, J M, Lei, Y, Leich, H, Leiste, R, Levtchenko, M, Levtchenko, P, Li, C, Li, L, Li, Z C, Likhoded, S, Lin, C H, Lin, W T, Linde, F L, Lista, L, Liu, Z A, Lohmann, W, Longo, E, Lu, Y S, Luci, C, Luminari, L, Lustermann, W, Ma, W G, Ma, X H, Ma, Y Q, Malgeri, L, Malinin, A, Mana, C, Mans, J, Martin, J P, Marzano, F, Mazumdar, K, McNeil, R R, Mele, S, Meng, X W, Merola, L, Meschini, M, Metzger, W J, Mihul, A, van Mil, A, Milcent, H, Mirabelli, G, Mnich, J, Mohanty, G B, Monteleoni, B, Muanza, y G S, Muijs, A J M, Musicar, B, Musy, M, Nagy, S, Nahnhauer, R, Naumov, V A, Natale, S, Napolitano, M, Nessi-Tedaldi, F, Newman, H, Nisati, A, Novak, T, Kluge, Hannelies, Ofierzynski, R, Organtini, G, Pal, I, Palomares, C, Paolucci, P, Paramatti, R, Parriaud, J -F, Passaleva, G, Patricelli, S, Paul, Thomas Cantzon, Pauluzzi, M, Paus, C, Pauss, F, Pedace, M, Pensotti, S, Perret-Gallix, D, Petersen, B, Piccolo, D, Pierella, F, Pieri, M, Pioppi, M, Piroue, P A, Pistolesi, E, Plyaskin, V, Pohl, M, Pojidaev, V, Pothier, J, Prokofev, D, Quartieri, J, Qing, C R, Rahal-Callot, G, Rahaman, Mohammad Azizur, Raics, P, Raja, N, Ramelli, R, Rancoita, P G, Ranieri, R, Raspereza, A, Ravindran, K C, Razis, P, Ren, D, Rescigno, M, Reucroft, S, Rewiersma, P, Riemann, y S, Riles, Keith, Roe, B P, Rojkov, A, Romero, L, Rosca, A, Rosemann, C, Rosenbleck, C, Rosier-Lees, S, Roth, Stefan, Rubio, J A, Ruggiero, G, Rykaczewski, H, Saidi, R, Sakharov, A, Saremi, S, Sarkar, S, Salicio, J, Sanchez, E, Schafer, C, Schegelsky, V, Schmitt, V, Schoeneich, B, Schopper, H, Schotanus, D J, Sciacca, C, Servoli, L, Shen, C Q, Shevchenko, S, Shivarov, N, Shoutko, V, Shumilov, E, Shvorob, A, Son, D, Souga, C, Spillantini, P, Steuer, M, Stickland, D P, Stoyanov, B, Straessner, A, Sudhakar, K, Sulanke, H, Sultanov, G, Sun, L Z, Sushkov, S, Suter, H, Swain, J D, Szillasi, Z, Tang, X W, Tarjan, P, Tauscher, L, Taylor, L, Tellili, B, Teyssier, D, Timmermans, Charles, Ting, Samuel C C, Ting, S M, Tonwar, S C, Toth, J, Trowitzsch, G, Tully, C, Tung, K L, Ulbricht, J, Unger, M, Valente, E, Verkooijen, H, Van de Walle, R T, Vasquez, R, Veszpremi, V, Vesztergombi, G, Vetlitsky, I, Vicinanza, D, Viertel, G, Villa, S, Vivargent, M, Vlachos, S, Vodopianov, I, Vogel, H, Vogt, H, Vorobev, I, Vorobyov, A A, Wadhwa, M, Wang, R G, Wang, Q, Wang, X L, Wang, X W, Wang, Z M, Weber, M, van Wijk, R, Wijnen, T A M, Wilkens, H, Wynhoff, S, Xia, L, Xu, Y P, Xu, J S, Xu, Z Z, Yamamoto, J, Yang, B Z, Yang, C G, Yang, H J, Yang, M, Yang, X F, Yao, Z G, Yeh, S C, Yu, Z Q, Zalite, An, Zalite, Yu, Zhang, C, Zhang, F, Zhang, J, Zhang, S, Zhang, Z P, Zhao, J, Zhou, S J, Zhu, G Y, Zhu, R Y, Zhuang, H L, Zhu, Q Q, Zichichi, A, Zimmermann, B, Zoller, M, Zwart, A N M, L3 (IHEF, IoP, FNWI), Achard, P, Adriani, O, Aguilar Benitez, M, van den Akker, M, Alcaraz, J, Alemanni, G, Allaby, J, Aloisio, A, Alviggi, M, Anderhub, H, Andreev, V, Anselmo, F, Arefiev, A, Azemoon, T, Aziz, T, Bagnaia, P, Bajo, A, Baksay, G, Baksay, L, Bähr, J, Baldew, S, Banerjee, S, Barczyk, A, Barillère, R, Bartalini, P, Basile, M, Batalova, N, Battiston, R, Bay, A, Becattini, F, Becker, U, Behner, F, Bellucci, L, Berbeco, R, Berdugo, J, Berges, P, Bertucci, B, Betev, B, Biasini, M, Biglietti, M, Biland, A, Blaising, J, Blyth, S, Bobbink, G, Böhm, A, Boldizsar, L, Borgia, B, Bottai, S, Bourilkov, D, Bourquin, M, Braccini, S, Branson, J, Brochu, F, Burger, J, Burger, W, Cai, X, Capell, M, Cara Romeo, G, Carlino, G, Cartacci, A, Casaus, J, Cavallari, F, Cavallo, N, Cecchi, C, Cerrada, M, Chamizo, M, Chang, Y, Chemarin, M, Chen, A, Chen, G, Chen, H, Chiarusi, T, Chiefari, G, Cifarelli, L, Cindolo, F, Clare, I, Clare, R, Coignet, G, Colino, N, Costantini, S, de la Cruz, B, Cucciarelli, S, de Asmundis, R, Déglon, P, Debreczeni, J, Degré, A, Dehmelt, K, Deiters, K, della Volpe, D, Delmeire, E, Denes, P, Denotaristefani, F, De Salvo, A, Diemoz, M, Dierckxsens, M, Ding, L, Dionisi, C, Dittmar, M, Doria, A, Dova, M, Duchesneau, D, Duda, M, Duran, I, Echenard, B, Eline, A, El Mamouni, H, Engler, A, Eppling, F, Extermann, P, Faber, G, Falagan, M, Falciano, S, Favara, A, Fay, J, Fedin, O, Felcini, M, Ferguson, T, Fiandrini, E, Field, J, Filthaut, F, Fisher, W, Forconi, G, Freudenreich, K, Furetta, C, Galaktionov, Y, Ganguli, S, Garcia Abia, P, Gataullin, M, Gentile, S, Giagu, S, Gong, Z, Grabosch, H, Grenier, G, Grimm, O, Groenstege, H, Gruenewald, M, Guo, Y, Gupta, S, Gupta, V, Gurtu, A, Gutay, L, Haas, D, Haller, C, Hatzifotiadou, D, Hayashi, Y, He, Z, Hebbeker, T, Hervé, A, Hirschfelder, J, Hofer, H, Hoferjun, H, Hohlmann, M, Holzner, G, Hou, S, Huo, A, Ito, N, Jin, B, Jindal, P, Jing, C, Jones, L, de Jong, P, Josa Mutuberría, I, Kantserov, V, Kaur, M, Kawakami, S, Kienzle Focacci, M, Kim, J, Kirkby, J, Kittel, W, Klimentov, A, König, A, Kok, E, Korn, A, Kopal, M, Koutsenko, V, Kräber, M, Kuang, H, Kraemer, R, Krüger, A, Kuijpers, J, Kunin, A, Ladron de Guevara, P, Laktineh, I, Landi, G, Lebeau, M, Lebedev, A, Lebrun, P, Lecomte, P, Lecoq, P, Le Coultre, P, Le Goff, J, Lei, Y, Leich, H, Leiste, R, Levtchenko, M, Levtchenko, P, Li, C, Li, L, Li, Z, Likhoded, S, Lin, C, Lin, W, Linde, F, Lista, L, Liu, Z, Lohmann, W, Longo, E, Lu, Y, Luci, C, Luminari, L, Lustermann, W, Ma, W, Ma, X, Ma, Y, Malgeri, L, Malinin, A, Maña, C, Mans, J, Martin, J, Marzano, F, Mazumdar, K, Mcneil, R, Mele, S, Meng, X, Merola, L, Meschini, M, Metzger, W, Mihul, A, van Mil, A, Milcent, H, Mirabelli, G, Mohanty, G, Monteleoni, B, Muanza, G, Muijs, A, Musy, M, Nagy, S, Nahnhauer, R, Naumov, V, Natale, S, Napolitano, M, Nessi Tedaldi, F, Newman, H, Nisati, A, Novak, T, Nowak, H, Ofierzynski, R, Organtini, G, Pal, I, Palomares, C, Paolucci, P, Paramatti, R, Parriaud, J, Passaleva, G, Patricelli, S, Paul, T, Pauluzzi, M, Paus, C, Pauss, F, Pedace, M, Pensotti, S, Perret Gallix, D, Petersen, B, Piccolo, D, Pierella, F, Pieri, M, Pioppi, M, Piroué, P, Pistolesi, E, Plyaskin, V, Pohl, M, Pojidaev, V, Pothier, J, Prokofiev, D, Qing, C, Rahal Callot, G, Rahaman, M, Raics, P, Raja, N, Ramelli, R, Rancoita, P, Ranieri, R, Raspereza, A, Ravindran, K, Razis, P, Rembeczki, S, Ren, D, Rescigno, M, Reucroft, S, Rewiersma, P, Riemann, S, Riles, K, Roe, B, Rojkov, A, Romero, L, Rosca, A, Rosier Lees, S, Roth, S, Rubio, J, Ruggiero, G, Rykaczewski, H, Saidi, R, Sakharov, A, Saremi, S, Sarkar, S, Salicio, J, Sanchez, E, Schäfer, C, Schegelsky, V, Schmitt, V, Schoeneich, B, Schopper, H, Schotanus, D, Sciacca, C, Servoli, L, Shen, C, Shevchenko, S, Shivarov, N, Shoutko, V, Shumilov, E, Shvorob, A, Son, D, Souga, C, Spillantini, P, Steuer, M, Stickland, D, Stoyanov, B, Straessner, A, Sudhakar, K, Sulanke, H, Sultanov, G, Sun, L, Suter, H, Swain, J, Szillasi, Z, Tang, X, Tarjan, P, Tauscher, L, Taylor, L, Tellili, B, Teyssier, D, Timmermans, C, Ting, S, Tonwar, S, Tóth, J, Trowitzsch, G, Tully, C, Tung, K, Ulbricht, J, Unger, M, Valente, E, Verkooijen, H, Van de Walle, R, Vasquez, R, Vesztergombi, G, Vetlitsky, I, Viertel, G, Vivargent, M, Vlachos, S, Vodopianov, I, Vogel, H, Vogt, H, Vorobiev, I, Vorobyov, A, Wadhwa, M, Wang, R, Wang, Q, Wang, X, Wang, Z, Weber, M, van Wijk, R, Wijnen, T, Wilkens, H, Wynhoff, S, Xia, L, Xu, Y, Xu, J, Xu, Z, Yamamoto, J, Yang, B, Yang, C, Yang, H, Yang, M, Yang, X, Yao, Z, Yeh, S, Yu, Z, Zalite, A, Zalite, Y, Zhang, C, Zhang, F, Zhang, J, Zhang, S, Zhang, Z, Zhao, J, Zhou, S, Zhu, G, Zhu, R, Zhu, Q, Zhuang, H, Zichichi, A, Zimmermann, B, Zöller, M, Zwart, A, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National 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Subjects
ISM: cosmic rays, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, L3+C, Cosmic Rays, Cosmic ray, Context (language use), Astrophysics, ddc:500.2, Sun: solar wind, 01 natural sciences, 7. Clean energy, law.invention, FIS/05 - ASTRONOMIA E ASTROFISICA, plasmas, sun : magnetic fields, Sun : solar wind, interplanetary, medium, ISM : cosmic rays, Astronomy & Astrophysics, law, Solar wind(sun), Magnetic fields(sun), 0103 physical sciences, cosmic rays [ISM], [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], 010306 general physics, Anisotropy, Collider, 010303 astronomy & astrophysics, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), Sun: magnetic fields, Ciencias Exactas, Physics, Large Hadron Collider, Muon, Isotropy, Astronomy and Astrophysics, solar wind [Sun], magnetic fields [Sun], Space and Planetary Science, Sidereal time, Plasmas, Experimental High Energy Physics, ddc:520, High Energy Physics::Experiment, Particle Physics - Experiment, FIS/04 - FISICA NUCLEARE E SUBNUCLEARE, Interplanetary medium
Abstract

Context. Primary cosmic rays experience multiple deflections in the non-uniform galactic and heliospheric magnetic fields which may generate anisotropies. Aims. A study of anisotropies in the energy range between 100 and 500 GeV is performed. This energy range is not yet well explored. Methods. The L3 detector at the CERN electron-positron collider, LEP, is used for a study of the angular distribution of atmospheric muons with energies above 20 GeV. This distribution is used to investigate the isotropy of the time-dependent intensity of the primary cosmic-ray flux with a Fourier analysis. Results. A small deviation from isotropy at energies around 200 GeV is observed for the second harmonics at the solar frequency. No sidereal anisotropy is found at a level above 10-4 . The measurements were performed in the years 1999 and 2000., La lista completa de autores que integran el documento puede consultarse en el archivo., Facultad de Ciencias Exactas

Published
2008

9. An analysis of unidimensional soliton gas models of magnetohydrodynamic turbulence in thf solar wind

Author

Dawson, S.P. and Fontán, C.F.

Subjects
Hydromagnetics, solar wind [Sun]
Abstract

We compare two statistical models of Alfvén solitons whose evolution is described by the one-dimensional derivative nonlinear Schrödinger (DNLS) equation, contrasting their predictions with solar wind observations. Both distribution functions give the same mean number of solitons. This confirms a previous calculation of Ponce Dawson and Ferro FontÁn of the number of solitons which evolve from an arbitrary initial condition. One of the distribution functions follows an exponential law with soliton energy and the other follows a power law; the latter gives better results than the former. Within these models, we can explain the variation of the observed spectra (spectral index, outer scale, and maximum value) with the heliocentric distance. This variation is related to the radial dependence of the mean level of modulational instability in the medium. Concerning the spectral index, our calculation improves that of Ovenden, Shah, and Schwartz, because an average over the soliton phases is included. Fil:Dawson, S.P. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.

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