Anisotropy of the magnetic correlation function in the inner heliosphere
For over four decades, low frequency plasma and electromagnetic fluctuations have been observed in the solar wind (SW), making it the most completely studied case of magnetohydrodynamic turbulence in astrophysics, and the only one extensively and directly studied using in situ observations. Magnetoh...
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| Formato: | Documento de conferencia publishedVersion |
| Lenguaje: | Inglés |
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2010
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| Acceso en línea: | http://hdl.handle.net/20.500.12110/paper_0094243X_v1216_n_p160_Ruiz |
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paperaa:paper_0094243X_v1216_n_p160_Ruiz2023-06-12T16:46:04Z Anisotropy of the magnetic correlation function in the inner heliosphere AIP Conf. Proc. 2010;1216:160-163 Ruiz, M.E. Dasso, S. Matthaeus, W.H. Marsch, E. Weygand, J.M. Magnetic anisotropies Magnetohydrodynamical turbulence Solar wind For over four decades, low frequency plasma and electromagnetic fluctuations have been observed in the solar wind (SW), making it the most completely studied case of magnetohydrodynamic turbulence in astrophysics, and the only one extensively and directly studied using in situ observations. Magnetohydrodynamic scale fluctuations in the SW are usually anisotropic with respect to the local mean magnetic field (B0). In this work, we present a study of turbulent properties in the inner heliosphere (solar wind between 0.3 and 1 AU) based on modeling in situ plasma and magnetic observations collected by Helios 1 and Helios 2 spacecraft throughout a solar minimum. We present preliminary results on the evolution of the spatial structure of the magnetic self-correlation function in the inner heliosphere. In particular we focus on the evolution of the integral length scale (λ) for magnetic fluctuations and on its anisotropy in the inertial range. As previously known from different studies, we confirm that near Earth λ ∥>λ⊥ (with λ∥ and λ⊥ representing the integral length in the parallel and perpendicular directions respect to B0, respectively). However, for lower distances to the Sun we found that λ∥<λ ⊥. Results presented here will help us to refine models used to describe the turbulence and waves activity in the inner heliosphere. © 2010 American Institute of Physics. Fil:Ruiz, M.E. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Dasso, S. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. 2010 info:eu-repo/semantics/conferenceObject info:ar-repo/semantics/documento de conferencia info:eu-repo/semantics/publishedVersion application/pdf eng info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_0094243X_v1216_n_p160_Ruiz |
| institution |
Universidad de Buenos Aires |
| institution_str |
I-28 |
| repository_str |
R-134 |
| collection |
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) |
| language |
Inglés |
| orig_language_str_mv |
eng |
| topic |
Magnetic anisotropies Magnetohydrodynamical turbulence Solar wind |
| spellingShingle |
Magnetic anisotropies Magnetohydrodynamical turbulence Solar wind Ruiz, M.E. Dasso, S. Matthaeus, W.H. Marsch, E. Weygand, J.M. Anisotropy of the magnetic correlation function in the inner heliosphere |
| topic_facet |
Magnetic anisotropies Magnetohydrodynamical turbulence Solar wind |
| description |
For over four decades, low frequency plasma and electromagnetic fluctuations have been observed in the solar wind (SW), making it the most completely studied case of magnetohydrodynamic turbulence in astrophysics, and the only one extensively and directly studied using in situ observations. Magnetohydrodynamic scale fluctuations in the SW are usually anisotropic with respect to the local mean magnetic field (B0). In this work, we present a study of turbulent properties in the inner heliosphere (solar wind between 0.3 and 1 AU) based on modeling in situ plasma and magnetic observations collected by Helios 1 and Helios 2 spacecraft throughout a solar minimum. We present preliminary results on the evolution of the spatial structure of the magnetic self-correlation function in the inner heliosphere. In particular we focus on the evolution of the integral length scale (λ) for magnetic fluctuations and on its anisotropy in the inertial range. As previously known from different studies, we confirm that near Earth λ ∥>λ⊥ (with λ∥ and λ⊥ representing the integral length in the parallel and perpendicular directions respect to B0, respectively). However, for lower distances to the Sun we found that λ∥<λ ⊥. Results presented here will help us to refine models used to describe the turbulence and waves activity in the inner heliosphere. © 2010 American Institute of Physics. |
| format |
Documento de conferencia Documento de conferencia publishedVersion |
| author |
Ruiz, M.E. Dasso, S. Matthaeus, W.H. Marsch, E. Weygand, J.M. |
| author_facet |
Ruiz, M.E. Dasso, S. Matthaeus, W.H. Marsch, E. Weygand, J.M. |
| author_sort |
Ruiz, M.E. |
| title |
Anisotropy of the magnetic correlation function in the inner heliosphere |
| title_short |
Anisotropy of the magnetic correlation function in the inner heliosphere |
| title_full |
Anisotropy of the magnetic correlation function in the inner heliosphere |
| title_fullStr |
Anisotropy of the magnetic correlation function in the inner heliosphere |
| title_full_unstemmed |
Anisotropy of the magnetic correlation function in the inner heliosphere |
| title_sort |
anisotropy of the magnetic correlation function in the inner heliosphere |
| publishDate |
2010 |
| url |
http://hdl.handle.net/20.500.12110/paper_0094243X_v1216_n_p160_Ruiz |
| work_keys_str_mv |
AT ruizme anisotropyofthemagneticcorrelationfunctionintheinnerheliosphere AT dassos anisotropyofthemagneticcorrelationfunctionintheinnerheliosphere AT matthaeuswh anisotropyofthemagneticcorrelationfunctionintheinnerheliosphere AT marsche anisotropyofthemagneticcorrelationfunctionintheinnerheliosphere AT weygandjm anisotropyofthemagneticcorrelationfunctionintheinnerheliosphere |
| _version_ |
1769810174730567680 |