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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Autores principales:	Gómez, D., Martín, L.N., Dmitruk, P.
Formato:	JOUR
Materias:	Magnetohydrodynamics Solar physics Space physics Turbulence Coronal active regions Electromagnetic spectra High resolution observations Ionized hydrogen plasmas Mean magnetic field Reduced magnetohydrodynamics Solar wind Sun
Acceso en línea:	http://hdl.handle.net/20.500.12110/paper_02731177_v51_n10_p1916_Gomez
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	todo:paper_02731177_v51_n10_p1916_Gomez
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spelling	todo:paper_02731177_v51_n10_p1916_Gomez2023-10-03T15:15:44Z Magnetohydrodynamics in solar and space physics Gómez, D. Martín, L.N. Dmitruk, P. 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. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar 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 Gómez, D. Martín, L.N. Dmitruk, P. 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.
format	JOUR
author	Gómez, D. Martín, L.N. Dmitruk, P.
author_facet	Gómez, D. Martín, L.N. Dmitruk, P.
author_sort	Gómez, D.
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
url	http://hdl.handle.net/20.500.12110/paper_02731177_v51_n10_p1916_Gomez
work_keys_str_mv	AT gomezd magnetohydrodynamicsinsolarandspacephysics AT martinln magnetohydrodynamicsinsolarandspacephysics AT dmitrukp magnetohydrodynamicsinsolarandspacephysics
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Magnetohydrodynamics in solar and space physics

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