Magnetohydrodynamics in solar and space physics
Because of its proximity, our Sun provides a unique opportunity to perform high resolution observations of its outer layers throughout the whole electromagnetic spectrum. We can also theoretically model most of the fascinating physical phenomena taking place on the Sun, as well as their impact on th...
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Acceso en línea: | https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_02731177_v51_n10_p1916_Gomez http://hdl.handle.net/20.500.12110/paper_02731177_v51_n10_p1916_Gomez |
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paper:paper_02731177_v51_n10_p1916_Gomez2023-06-08T15:25:42Z Magnetohydrodynamics in solar and space physics Gomez, Daniel Osvaldo Dmitruk, Pablo Ariel Magnetohydrodynamics Solar physics Space physics Turbulence Coronal active regions Electromagnetic spectra High resolution observations Ionized hydrogen plasmas Mean magnetic field Reduced magnetohydrodynamics Solar physics Space physics Solar wind Sun Turbulence Magnetohydrodynamics Because of its proximity, our Sun provides a unique opportunity to perform high resolution observations of its outer layers throughout the whole electromagnetic spectrum. We can also theoretically model most of the fascinating physical phenomena taking place on the Sun, as well as their impact on the solar system. Many of these phenomena can be properly studied within the framework of magnetohydrodynamics. More specifically, we assume a fully ionized hydrogen plasma and adopt the more comprehensive two-fluid magnetohydrodynamic approximation. For problems such as the solar wind or magnetic loops in the solar corona, which are shaped by a relatively strong mean magnetic field, the reduced magnetohydrodynamic approximation is often used. We will review the basic features of both two-fluid and one-fluid magnetohydrodynamics, and focus on two particular applications: the turbulent heating of coronal active regions and the dynamics of the solar wind.© 2012 COSPAR. Published by Elsevier Ltd. All rights reserved. Fil:Gómez, D. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Dmitruk, P. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. 2013 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_02731177_v51_n10_p1916_Gomez http://hdl.handle.net/20.500.12110/paper_02731177_v51_n10_p1916_Gomez |
institution |
Universidad de Buenos Aires |
institution_str |
I-28 |
repository_str |
R-134 |
collection |
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) |
topic |
Magnetohydrodynamics Solar physics Space physics Turbulence Coronal active regions Electromagnetic spectra High resolution observations Ionized hydrogen plasmas Mean magnetic field Reduced magnetohydrodynamics Solar physics Space physics Solar wind Sun Turbulence Magnetohydrodynamics |
spellingShingle |
Magnetohydrodynamics Solar physics Space physics Turbulence Coronal active regions Electromagnetic spectra High resolution observations Ionized hydrogen plasmas Mean magnetic field Reduced magnetohydrodynamics Solar physics Space physics Solar wind Sun Turbulence Magnetohydrodynamics Gomez, Daniel Osvaldo Dmitruk, Pablo Ariel Magnetohydrodynamics in solar and space physics |
topic_facet |
Magnetohydrodynamics Solar physics Space physics Turbulence Coronal active regions Electromagnetic spectra High resolution observations Ionized hydrogen plasmas Mean magnetic field Reduced magnetohydrodynamics Solar physics Space physics Solar wind Sun Turbulence Magnetohydrodynamics |
description |
Because of its proximity, our Sun provides a unique opportunity to perform high resolution observations of its outer layers throughout the whole electromagnetic spectrum. We can also theoretically model most of the fascinating physical phenomena taking place on the Sun, as well as their impact on the solar system. Many of these phenomena can be properly studied within the framework of magnetohydrodynamics. More specifically, we assume a fully ionized hydrogen plasma and adopt the more comprehensive two-fluid magnetohydrodynamic approximation. For problems such as the solar wind or magnetic loops in the solar corona, which are shaped by a relatively strong mean magnetic field, the reduced magnetohydrodynamic approximation is often used. We will review the basic features of both two-fluid and one-fluid magnetohydrodynamics, and focus on two particular applications: the turbulent heating of coronal active regions and the dynamics of the solar wind.© 2012 COSPAR. Published by Elsevier Ltd. All rights reserved. |
author |
Gomez, Daniel Osvaldo Dmitruk, Pablo Ariel |
author_facet |
Gomez, Daniel Osvaldo Dmitruk, Pablo Ariel |
author_sort |
Gomez, Daniel Osvaldo |
title |
Magnetohydrodynamics in solar and space physics |
title_short |
Magnetohydrodynamics in solar and space physics |
title_full |
Magnetohydrodynamics in solar and space physics |
title_fullStr |
Magnetohydrodynamics in solar and space physics |
title_full_unstemmed |
Magnetohydrodynamics in solar and space physics |
title_sort |
magnetohydrodynamics in solar and space physics |
publishDate |
2013 |
url |
https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_02731177_v51_n10_p1916_Gomez http://hdl.handle.net/20.500.12110/paper_02731177_v51_n10_p1916_Gomez |
work_keys_str_mv |
AT gomezdanielosvaldo magnetohydrodynamicsinsolarandspacephysics AT dmitrukpabloariel magnetohydrodynamicsinsolarandspacephysics |
_version_ |
1768544500950499328 |