Instabilities; shocks and turbulence in space and astrophysical plasmas

Autores
Gomez, Daniel Osvaldo
Año de publicación
2018
Idioma
español castellano
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The dynamics of plasmas pervading the interplanetary and interstellar medium are often described within the frame of magnetohydrodynamics (MHD), which involves the coupling between flows and magnetic fields. This theoretical framework adequately models the large scale behavior of a number of processes taking place in these plasmas, such as the generation of magnetic fields by dynamo mechanisms, the impulsive release of magnetic energy in reconnection events or the complex dynamics of turbulent flows. However, there are physical phenomena at smaller spatial scales that cannot be explained within the framework of traditional MHD. Throughout this work we show that the inclusion of additional physical effects such as the Hall current or electron inertia, it becomes possible to describe phenomena such as the fine structure of some shocks or the recently observed deviations in the turbulent energy spectrum of the solar wind.
Fil: Gomez, Daniel Osvaldo. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Materia
PLASMAS
INSTABILITIES
SHOCKS
TURBULENCE
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/86294
Acceder
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repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Instabilities; shocks and turbulence in space and astrophysical plasmasGomez, Daniel OsvaldoPLASMASINSTABILITIESSHOCKSTURBULENCEhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The dynamics of plasmas pervading the interplanetary and interstellar medium are often described within the frame of magnetohydrodynamics (MHD), which involves the coupling between flows and magnetic fields. This theoretical framework adequately models the large scale behavior of a number of processes taking place in these plasmas, such as the generation of magnetic fields by dynamo mechanisms, the impulsive release of magnetic energy in reconnection events or the complex dynamics of turbulent flows. However, there are physical phenomena at smaller spatial scales that cannot be explained within the framework of traditional MHD. Throughout this work we show that the inclusion of additional physical effects such as the Hall current or electron inertia, it becomes possible to describe phenomena such as the fine structure of some shocks or the recently observed deviations in the turbulent energy spectrum of the solar wind.Fil: Gomez, Daniel Osvaldo. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaAsociación Argentina de Astronomía2018-10info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/86294Gomez, Daniel Osvaldo; Instabilities; shocks and turbulence in space and astrophysical plasmas; Asociación Argentina de Astronomía; Boletín de la Asociación Argentina de Astronomía; 60; 10-2018; 195-2000571-3285CONICET DigitalCONICETspainfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-03T09:55:36Zoai:ri.conicet.gov.ar:11336/86294instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-03 09:55:36.426CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Instabilities; shocks and turbulence in space and astrophysical plasmas
title Instabilities; shocks and turbulence in space and astrophysical plasmas
spellingShingle Instabilities; shocks and turbulence in space and astrophysical plasmas
Gomez, Daniel Osvaldo
PLASMAS
INSTABILITIES
SHOCKS
TURBULENCE
title_short Instabilities; shocks and turbulence in space and astrophysical plasmas
title_full Instabilities; shocks and turbulence in space and astrophysical plasmas
title_fullStr Instabilities; shocks and turbulence in space and astrophysical plasmas
title_full_unstemmed Instabilities; shocks and turbulence in space and astrophysical plasmas
title_sort Instabilities; shocks and turbulence in space and astrophysical plasmas
dc.creator.none.fl_str_mv Gomez, Daniel Osvaldo
author Gomez, Daniel Osvaldo
author_facet Gomez, Daniel Osvaldo
author_role author
dc.subject.none.fl_str_mv PLASMAS
INSTABILITIES
SHOCKS
TURBULENCE
topic PLASMAS
INSTABILITIES
SHOCKS
TURBULENCE
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv The dynamics of plasmas pervading the interplanetary and interstellar medium are often described within the frame of magnetohydrodynamics (MHD), which involves the coupling between flows and magnetic fields. This theoretical framework adequately models the large scale behavior of a number of processes taking place in these plasmas, such as the generation of magnetic fields by dynamo mechanisms, the impulsive release of magnetic energy in reconnection events or the complex dynamics of turbulent flows. However, there are physical phenomena at smaller spatial scales that cannot be explained within the framework of traditional MHD. Throughout this work we show that the inclusion of additional physical effects such as the Hall current or electron inertia, it becomes possible to describe phenomena such as the fine structure of some shocks or the recently observed deviations in the turbulent energy spectrum of the solar wind.
Fil: Gomez, Daniel Osvaldo. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
description The dynamics of plasmas pervading the interplanetary and interstellar medium are often described within the frame of magnetohydrodynamics (MHD), which involves the coupling between flows and magnetic fields. This theoretical framework adequately models the large scale behavior of a number of processes taking place in these plasmas, such as the generation of magnetic fields by dynamo mechanisms, the impulsive release of magnetic energy in reconnection events or the complex dynamics of turbulent flows. However, there are physical phenomena at smaller spatial scales that cannot be explained within the framework of traditional MHD. Throughout this work we show that the inclusion of additional physical effects such as the Hall current or electron inertia, it becomes possible to describe phenomena such as the fine structure of some shocks or the recently observed deviations in the turbulent energy spectrum of the solar wind.
publishDate 2018
dc.date.none.fl_str_mv 2018-10
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/86294
Gomez, Daniel Osvaldo; Instabilities; shocks and turbulence in space and astrophysical plasmas; Asociación Argentina de Astronomía; Boletín de la Asociación Argentina de Astronomía; 60; 10-2018; 195-200
0571-3285
CONICET Digital
CONICET
url http://hdl.handle.net/11336/86294
identifier_str_mv Gomez, Daniel Osvaldo; Instabilities; shocks and turbulence in space and astrophysical plasmas; Asociación Argentina de Astronomía; Boletín de la Asociación Argentina de Astronomía; 60; 10-2018; 195-200
0571-3285
CONICET Digital
CONICET
dc.language.none.fl_str_mv spa
language spa
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv Asociación Argentina de Astronomía
publisher.none.fl_str_mv Asociación Argentina de Astronomía
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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score 13.13397

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