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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/76866
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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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1844613952292519936 |
score |
13.070432 |