Coronal heating by surface Alfvén wave damping: Implementation in a global magnetohydrodynamics model of the solar wind

Autores
Evans, Rebekah M.; Opher, M.; Oran, R.; van der Holst, Bartholomeus; Sokolov, I.V.; Frazin, Richard A.; Gombosi, Tamas I.; Vasquez, Alberto Marcos
Año de publicación
2012
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The heating and acceleration of the solar wind is an active area of research. Alfvén waves, because of their ability to accelerate and heat the plasma, are a likely candidate in both processes. Many models have explored wave dissipation mechanisms which act either in closed or open magnetic field regions. In this work, we emphasize the boundary between these regions, drawing on observations which indicate unique heating is present there. We utilize a new solar corona component of the Space Weather Modeling Framework, in which Alfvén wave energy transport is self-consistently coupled to the magnetohydrodynamic equations. In this solar wind model, the wave pressure gradient accelerates and wave dissipation heats the plasma. Kolmogorov-like wave dissipation as expressed by Hollweg along open magnetic field lines was presented in van der Holst et al. Here, we introduce an additional dissipation mechanism: surface Alfvén wave (SAW) damping, which occurs in regions with transverse (with respect to the magnetic field) gradients in the local Alfvén speed. For solar minimum conditions, we find that SAW dissipation is weak in the polar regions (where Hollweg dissipation is strong), and strong in subpolar latitudes and the boundaries of open and closed magnetic fields (where Hollweg dissipation is weak). We show that SAW damping reproduces regions of enhanced temperature at the boundaries of open and closed magnetic fields seen in tomographic reconstructions in the low corona. Also, we argue that Ulysses data in the heliosphere show enhanced temperatures at the boundaries of fast and slow solar wind, which is reproduced by SAW dissipation. Therefore, the model's temperature distribution shows best agreement with these observations when both dissipation mechanisms are considered. Lastly, we use observational constraints of shock formation in the low corona to assess the Alfvén speed profile in the model. We find that, compared to a polytropic solar wind model, the wave-driven model with physical dissipation mechanisms presented in this work is more aligned with an empirical Alfvén speed profile. Therefore, a wave-driven model which includes the effects of SAW damping is a better background to simulate coronal-mass-ejection-driven shocks. © 2012. The American Astronomical Society. All rights reserved.
Fil: Evans, Rebekah M.. Boston University; Estados Unidos
Fil: Opher, M.. Boston University; Estados Unidos
Fil: Oran, R.. University Of Michigan, Ann Arbor; Estados Unidos
Fil: van der Holst, Bartholomeus. University Of Michigan, Ann Arbor; Estados Unidos
Fil: Sokolov, I.V.. University Of Michigan, Ann Arbor; Estados Unidos
Fil: Frazin, Richard A.. University Of Michigan, Ann Arbor; Estados Unidos
Fil: Gombosi, Tamas I.. University Of Michigan, Ann Arbor; Estados Unidos
Fil: Vasquez, Alberto Marcos. 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
MAGNETIC FIELDS
MAGNETOHYDRODYNAMICS (MHD)
SOLAR WIND
SUN: CORONA
WAVES
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:11336/76866

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oai_identifier_str oai:ri.conicet.gov.ar:11336/76866
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repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Coronal heating by surface Alfvén wave damping: Implementation in a global magnetohydrodynamics model of the solar windEvans, Rebekah M.Opher, M.Oran, R.van der Holst, BartholomeusSokolov, I.V.Frazin, Richard A.Gombosi, Tamas I.Vasquez, Alberto MarcosMAGNETIC FIELDSMAGNETOHYDRODYNAMICS (MHD)SOLAR WINDSUN: CORONAWAVEShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The heating and acceleration of the solar wind is an active area of research. Alfvén waves, because of their ability to accelerate and heat the plasma, are a likely candidate in both processes. Many models have explored wave dissipation mechanisms which act either in closed or open magnetic field regions. In this work, we emphasize the boundary between these regions, drawing on observations which indicate unique heating is present there. We utilize a new solar corona component of the Space Weather Modeling Framework, in which Alfvén wave energy transport is self-consistently coupled to the magnetohydrodynamic equations. In this solar wind model, the wave pressure gradient accelerates and wave dissipation heats the plasma. Kolmogorov-like wave dissipation as expressed by Hollweg along open magnetic field lines was presented in van der Holst et al. Here, we introduce an additional dissipation mechanism: surface Alfvén wave (SAW) damping, which occurs in regions with transverse (with respect to the magnetic field) gradients in the local Alfvén speed. For solar minimum conditions, we find that SAW dissipation is weak in the polar regions (where Hollweg dissipation is strong), and strong in subpolar latitudes and the boundaries of open and closed magnetic fields (where Hollweg dissipation is weak). We show that SAW damping reproduces regions of enhanced temperature at the boundaries of open and closed magnetic fields seen in tomographic reconstructions in the low corona. Also, we argue that Ulysses data in the heliosphere show enhanced temperatures at the boundaries of fast and slow solar wind, which is reproduced by SAW dissipation. Therefore, the model's temperature distribution shows best agreement with these observations when both dissipation mechanisms are considered. Lastly, we use observational constraints of shock formation in the low corona to assess the Alfvén speed profile in the model. We find that, compared to a polytropic solar wind model, the wave-driven model with physical dissipation mechanisms presented in this work is more aligned with an empirical Alfvén speed profile. Therefore, a wave-driven model which includes the effects of SAW damping is a better background to simulate coronal-mass-ejection-driven shocks. © 2012. The American Astronomical Society. All rights reserved.Fil: Evans, Rebekah M.. Boston University; Estados UnidosFil: Opher, M.. Boston University; Estados UnidosFil: Oran, R.. University Of Michigan, Ann Arbor; Estados UnidosFil: van der Holst, Bartholomeus. University Of Michigan, Ann Arbor; Estados UnidosFil: Sokolov, I.V.. University Of Michigan, Ann Arbor; Estados UnidosFil: Frazin, Richard A.. University Of Michigan, Ann Arbor; Estados UnidosFil: Gombosi, Tamas I.. University Of Michigan, Ann Arbor; Estados UnidosFil: Vasquez, Alberto Marcos. 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; ArgentinaIOP Publishing2012-09info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/76866Evans, Rebekah M.; Opher, M.; Oran, R.; van der Holst, Bartholomeus; Sokolov, I.V.; et al.; Coronal heating by surface Alfvén wave damping: Implementation in a global magnetohydrodynamics model of the solar wind; IOP Publishing; Astrophysical Journal; 756; 2; 9-2012; 155-1680004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1088/0004-637X/756/2/155info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:08:26Zoai:ri.conicet.gov.ar:11336/76866instacron: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:34982025-09-29 10:08:26.322CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Coronal heating by surface Alfvén wave damping: Implementation in a global magnetohydrodynamics model of the solar wind
title Coronal heating by surface Alfvén wave damping: Implementation in a global magnetohydrodynamics model of the solar wind
spellingShingle Coronal heating by surface Alfvén wave damping: Implementation in a global magnetohydrodynamics model of the solar wind
Evans, Rebekah M.
MAGNETIC FIELDS
MAGNETOHYDRODYNAMICS (MHD)
SOLAR WIND
SUN: CORONA
WAVES
title_short Coronal heating by surface Alfvén wave damping: Implementation in a global magnetohydrodynamics model of the solar wind
title_full Coronal heating by surface Alfvén wave damping: Implementation in a global magnetohydrodynamics model of the solar wind
title_fullStr Coronal heating by surface Alfvén wave damping: Implementation in a global magnetohydrodynamics model of the solar wind
title_full_unstemmed Coronal heating by surface Alfvén wave damping: Implementation in a global magnetohydrodynamics model of the solar wind
title_sort Coronal heating by surface Alfvén wave damping: Implementation in a global magnetohydrodynamics model of the solar wind
dc.creator.none.fl_str_mv Evans, Rebekah M.
Opher, M.
Oran, R.
van der Holst, Bartholomeus
Sokolov, I.V.
Frazin, Richard A.
Gombosi, Tamas I.
Vasquez, Alberto Marcos
author Evans, Rebekah M.
author_facet Evans, Rebekah M.
Opher, M.
Oran, R.
van der Holst, Bartholomeus
Sokolov, I.V.
Frazin, Richard A.
Gombosi, Tamas I.
Vasquez, Alberto Marcos
author_role author
author2 Opher, M.
Oran, R.
van der Holst, Bartholomeus
Sokolov, I.V.
Frazin, Richard A.
Gombosi, Tamas I.
Vasquez, Alberto Marcos
author2_role author
author
author
author
author
author
author
dc.subject.none.fl_str_mv MAGNETIC FIELDS
MAGNETOHYDRODYNAMICS (MHD)
SOLAR WIND
SUN: CORONA
WAVES
topic MAGNETIC FIELDS
MAGNETOHYDRODYNAMICS (MHD)
SOLAR WIND
SUN: CORONA
WAVES
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 heating and acceleration of the solar wind is an active area of research. Alfvén waves, because of their ability to accelerate and heat the plasma, are a likely candidate in both processes. Many models have explored wave dissipation mechanisms which act either in closed or open magnetic field regions. In this work, we emphasize the boundary between these regions, drawing on observations which indicate unique heating is present there. We utilize a new solar corona component of the Space Weather Modeling Framework, in which Alfvén wave energy transport is self-consistently coupled to the magnetohydrodynamic equations. In this solar wind model, the wave pressure gradient accelerates and wave dissipation heats the plasma. Kolmogorov-like wave dissipation as expressed by Hollweg along open magnetic field lines was presented in van der Holst et al. Here, we introduce an additional dissipation mechanism: surface Alfvén wave (SAW) damping, which occurs in regions with transverse (with respect to the magnetic field) gradients in the local Alfvén speed. For solar minimum conditions, we find that SAW dissipation is weak in the polar regions (where Hollweg dissipation is strong), and strong in subpolar latitudes and the boundaries of open and closed magnetic fields (where Hollweg dissipation is weak). We show that SAW damping reproduces regions of enhanced temperature at the boundaries of open and closed magnetic fields seen in tomographic reconstructions in the low corona. Also, we argue that Ulysses data in the heliosphere show enhanced temperatures at the boundaries of fast and slow solar wind, which is reproduced by SAW dissipation. Therefore, the model's temperature distribution shows best agreement with these observations when both dissipation mechanisms are considered. Lastly, we use observational constraints of shock formation in the low corona to assess the Alfvén speed profile in the model. We find that, compared to a polytropic solar wind model, the wave-driven model with physical dissipation mechanisms presented in this work is more aligned with an empirical Alfvén speed profile. Therefore, a wave-driven model which includes the effects of SAW damping is a better background to simulate coronal-mass-ejection-driven shocks. © 2012. The American Astronomical Society. All rights reserved.
Fil: Evans, Rebekah M.. Boston University; Estados Unidos
Fil: Opher, M.. Boston University; Estados Unidos
Fil: Oran, R.. University Of Michigan, Ann Arbor; Estados Unidos
Fil: van der Holst, Bartholomeus. University Of Michigan, Ann Arbor; Estados Unidos
Fil: Sokolov, I.V.. University Of Michigan, Ann Arbor; Estados Unidos
Fil: Frazin, Richard A.. University Of Michigan, Ann Arbor; Estados Unidos
Fil: Gombosi, Tamas I.. University Of Michigan, Ann Arbor; Estados Unidos
Fil: Vasquez, Alberto Marcos. 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 heating and acceleration of the solar wind is an active area of research. Alfvén waves, because of their ability to accelerate and heat the plasma, are a likely candidate in both processes. Many models have explored wave dissipation mechanisms which act either in closed or open magnetic field regions. In this work, we emphasize the boundary between these regions, drawing on observations which indicate unique heating is present there. We utilize a new solar corona component of the Space Weather Modeling Framework, in which Alfvén wave energy transport is self-consistently coupled to the magnetohydrodynamic equations. In this solar wind model, the wave pressure gradient accelerates and wave dissipation heats the plasma. Kolmogorov-like wave dissipation as expressed by Hollweg along open magnetic field lines was presented in van der Holst et al. Here, we introduce an additional dissipation mechanism: surface Alfvén wave (SAW) damping, which occurs in regions with transverse (with respect to the magnetic field) gradients in the local Alfvén speed. For solar minimum conditions, we find that SAW dissipation is weak in the polar regions (where Hollweg dissipation is strong), and strong in subpolar latitudes and the boundaries of open and closed magnetic fields (where Hollweg dissipation is weak). We show that SAW damping reproduces regions of enhanced temperature at the boundaries of open and closed magnetic fields seen in tomographic reconstructions in the low corona. Also, we argue that Ulysses data in the heliosphere show enhanced temperatures at the boundaries of fast and slow solar wind, which is reproduced by SAW dissipation. Therefore, the model's temperature distribution shows best agreement with these observations when both dissipation mechanisms are considered. Lastly, we use observational constraints of shock formation in the low corona to assess the Alfvén speed profile in the model. We find that, compared to a polytropic solar wind model, the wave-driven model with physical dissipation mechanisms presented in this work is more aligned with an empirical Alfvén speed profile. Therefore, a wave-driven model which includes the effects of SAW damping is a better background to simulate coronal-mass-ejection-driven shocks. © 2012. The American Astronomical Society. All rights reserved.
publishDate 2012
dc.date.none.fl_str_mv 2012-09
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/11336/76866
Evans, Rebekah M.; Opher, M.; Oran, R.; van der Holst, Bartholomeus; Sokolov, I.V.; et al.; Coronal heating by surface Alfvén wave damping: Implementation in a global magnetohydrodynamics model of the solar wind; IOP Publishing; Astrophysical Journal; 756; 2; 9-2012; 155-168
0004-637X
CONICET Digital
CONICET
url http://hdl.handle.net/11336/76866
identifier_str_mv Evans, Rebekah M.; Opher, M.; Oran, R.; van der Holst, Bartholomeus; Sokolov, I.V.; et al.; Coronal heating by surface Alfvén wave damping: Implementation in a global magnetohydrodynamics model of the solar wind; IOP Publishing; Astrophysical Journal; 756; 2; 9-2012; 155-168
0004-637X
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1088/0004-637X/756/2/155
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 IOP Publishing
publisher.none.fl_str_mv IOP Publishing
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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