Anisotropy in fast and slow solar wind fluctuations
Using 5 years of spacecraft data from near Earth orbit, we investigate the correlation anisotropy of solar wind magnetohydrodynamic-scale fluctuations and show that the nature of the anisotropy differs in fast (>500 km s -1) and slow (<400 km s-1) streams. In particular, fast streams a...
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| Acceso en línea: | http://hdl.handle.net/20.500.12110/paper_0004637X_v635_n2II_pL181_Dasso |
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todo:paper_0004637X_v635_n2II_pL181_Dasso2023-10-03T14:02:00Z Anisotropy in fast and slow solar wind fluctuations Dasso, S. Milano, L.J. Matthaeus, W.H. Smith, C.W. MHD Plasmas Solar wind Turbulence Waves Using 5 years of spacecraft data from near Earth orbit, we investigate the correlation anisotropy of solar wind magnetohydrodynamic-scale fluctuations and show that the nature of the anisotropy differs in fast (>500 km s -1) and slow (<400 km s-1) streams. In particular, fast streams are relatively more dominated by fluctuations with wavevectors quasi-parallel to the local magnetic field, while slow streams, which appear to be more fully evolved turbulence, are more dominated by quasi-perpendicular fluctuation wavevectors. © 2005. The American Astronomical Society. All rights reserved. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_0004637X_v635_n2II_pL181_Dasso |
| institution |
Universidad de Buenos Aires |
| institution_str |
I-28 |
| repository_str |
R-134 |
| collection |
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) |
| topic |
MHD Plasmas Solar wind Turbulence Waves |
| spellingShingle |
MHD Plasmas Solar wind Turbulence Waves Dasso, S. Milano, L.J. Matthaeus, W.H. Smith, C.W. Anisotropy in fast and slow solar wind fluctuations |
| topic_facet |
MHD Plasmas Solar wind Turbulence Waves |
| description |
Using 5 years of spacecraft data from near Earth orbit, we investigate the correlation anisotropy of solar wind magnetohydrodynamic-scale fluctuations and show that the nature of the anisotropy differs in fast (>500 km s -1) and slow (<400 km s-1) streams. In particular, fast streams are relatively more dominated by fluctuations with wavevectors quasi-parallel to the local magnetic field, while slow streams, which appear to be more fully evolved turbulence, are more dominated by quasi-perpendicular fluctuation wavevectors. © 2005. The American Astronomical Society. All rights reserved. |
| format |
JOUR |
| author |
Dasso, S. Milano, L.J. Matthaeus, W.H. Smith, C.W. |
| author_facet |
Dasso, S. Milano, L.J. Matthaeus, W.H. Smith, C.W. |
| author_sort |
Dasso, S. |
| title |
Anisotropy in fast and slow solar wind fluctuations |
| title_short |
Anisotropy in fast and slow solar wind fluctuations |
| title_full |
Anisotropy in fast and slow solar wind fluctuations |
| title_fullStr |
Anisotropy in fast and slow solar wind fluctuations |
| title_full_unstemmed |
Anisotropy in fast and slow solar wind fluctuations |
| title_sort |
anisotropy in fast and slow solar wind fluctuations |
| url |
http://hdl.handle.net/20.500.12110/paper_0004637X_v635_n2II_pL181_Dasso |
| work_keys_str_mv |
AT dassos anisotropyinfastandslowsolarwindfluctuations AT milanolj anisotropyinfastandslowsolarwindfluctuations AT matthaeuswh anisotropyinfastandslowsolarwindfluctuations AT smithcw anisotropyinfastandslowsolarwindfluctuations |
| _version_ |
1807315570957221888 |