Shear-driven instabilities in hall-magnetohydrodynamic plasmas

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The large-scale dynamics of plasmas is well described within the framework of magnetohydrodynamics (MHD). However, whenever the ion density of the plasma becomes sufficiently low, the Hall effect is likely to become important. The role of the Hall effect has been studied in several astrophysical pla...

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Autores principales:	Bejarano, C., Gómez, D.O., Brandenburg, A.
Formato:	Artículo publishedVersion
Publicado:	2011
Acceso en línea:	http://hdl.handle.net/20.500.12110/paper_0004637X_v737_n2_p_Bejarano https://repositoriouba.sisbi.uba.ar/gsdl/cgi-bin/library.cgi?a=d&c=artiaex&d=paper_0004637X_v737_n2_p_Bejarano_oai
Aporte de:	Repositorio Digital de la Universidad de Buenos Aires (UBA) de Universidad de Buenos Aires

id	I28-R145-paper_0004637X_v737_n2_p_Bejarano_oai
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spelling	I28-R145-paper_0004637X_v737_n2_p_Bejarano_oai2024-08-16 Bejarano, C. Gómez, D.O. Brandenburg, A. 2011 The large-scale dynamics of plasmas is well described within the framework of magnetohydrodynamics (MHD). However, whenever the ion density of the plasma becomes sufficiently low, the Hall effect is likely to become important. The role of the Hall effect has been studied in several astrophysical plasma processes, such as magnetic reconnection, magnetic dynamo, MHD turbulence, or MHD instabilities. In particular, the development of small-scale instabilities is essential to understand the transport properties in a number of astrophysical plasmas. The magneto-rotational instability (MRI), which takes place in differentially rotating accretion disks embedded in relatively weak magnetic fields, is just one example. The influence of the large-scale velocity flows on small-scale instabilities is often approximated by a linear shear flow. In this paper, we quantitatively study the role of the Hall effect on plasmas embedded in large-scale shear flows. More precisely, we show that an instability develops when the Hall effect is present, which we therefore term as the Hall magneto-shear instability. As a particular case, we recover the so-called MRI and quantitatively assess the role of the Hall effect on its development and evolution. © 2011 The American Astronomical Society. All rights reserved. Fil:Bejarano, C. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Gómez, D.O. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. application/pdf http://hdl.handle.net/20.500.12110/paper_0004637X_v737_n2_p_Bejarano info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar Astrophys. J. 2011;737(2) Shear-driven instabilities in hall-magnetohydrodynamic plasmas info:eu-repo/semantics/article info:ar-repo/semantics/artículo info:eu-repo/semantics/publishedVersion https://repositoriouba.sisbi.uba.ar/gsdl/cgi-bin/library.cgi?a=d&c=artiaex&d=paper_0004637X_v737_n2_p_Bejarano_oai
institution	Universidad de Buenos Aires
institution_str	I-28
repository_str	R-145
collection	Repositorio Digital de la Universidad de Buenos Aires (UBA)
description	The large-scale dynamics of plasmas is well described within the framework of magnetohydrodynamics (MHD). However, whenever the ion density of the plasma becomes sufficiently low, the Hall effect is likely to become important. The role of the Hall effect has been studied in several astrophysical plasma processes, such as magnetic reconnection, magnetic dynamo, MHD turbulence, or MHD instabilities. In particular, the development of small-scale instabilities is essential to understand the transport properties in a number of astrophysical plasmas. The magneto-rotational instability (MRI), which takes place in differentially rotating accretion disks embedded in relatively weak magnetic fields, is just one example. The influence of the large-scale velocity flows on small-scale instabilities is often approximated by a linear shear flow. In this paper, we quantitatively study the role of the Hall effect on plasmas embedded in large-scale shear flows. More precisely, we show that an instability develops when the Hall effect is present, which we therefore term as the Hall magneto-shear instability. As a particular case, we recover the so-called MRI and quantitatively assess the role of the Hall effect on its development and evolution. © 2011 The American Astronomical Society. All rights reserved.
format	Artículo Artículo publishedVersion
author	Bejarano, C. Gómez, D.O. Brandenburg, A.
spellingShingle	Bejarano, C. Gómez, D.O. Brandenburg, A. Shear-driven instabilities in hall-magnetohydrodynamic plasmas
author_facet	Bejarano, C. Gómez, D.O. Brandenburg, A.
author_sort	Bejarano, C.
title	Shear-driven instabilities in hall-magnetohydrodynamic plasmas
title_short	Shear-driven instabilities in hall-magnetohydrodynamic plasmas
title_full	Shear-driven instabilities in hall-magnetohydrodynamic plasmas
title_fullStr	Shear-driven instabilities in hall-magnetohydrodynamic plasmas
title_full_unstemmed	Shear-driven instabilities in hall-magnetohydrodynamic plasmas
title_sort	shear-driven instabilities in hall-magnetohydrodynamic plasmas
publishDate	2011
url	http://hdl.handle.net/20.500.12110/paper_0004637X_v737_n2_p_Bejarano https://repositoriouba.sisbi.uba.ar/gsdl/cgi-bin/library.cgi?a=d&c=artiaex&d=paper_0004637X_v737_n2_p_Bejarano_oai
work_keys_str_mv	AT bejaranoc sheardriveninstabilitiesinhallmagnetohydrodynamicplasmas AT gomezdo sheardriveninstabilitiesinhallmagnetohydrodynamicplasmas AT brandenburga sheardriveninstabilitiesinhallmagnetohydrodynamicplasmas
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Shear-driven instabilities in hall-magnetohydrodynamic plasmas

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