A turbulence-driven model for heating and acceleration of the fast wind in coronal holes

Autores
Verdini, A.; Velli, M.; Matthaeus, W.H.; Oughton, S.; Dmitruk, P.
Año de publicación
2010
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
A model is presented for generation of fast solar wind in coronal holes, relying on heating that is dominated by turbulent dissipation of MHD fluctuations transported upward in the solar atmosphere. Scale-separated transport equations include large-scale fields, transverse Alfvénic fluctuations, and a small compressive dissipation due to parallel shears near the transition region. The model accounts for proton temperature, density, wind speed, and fluctuation amplitude as observed in remote sensing and in situ satellite data. © 2010. The American Astronomical Society. All rights reserved..
Fil:Dmitruk, P. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.
Fuente
Astrophys. J. Lett. 2010;708(2 PART 2):L116-L120
Materia
MHD
Solar wind
Turbulence
Waves
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by/2.5/ar
Repositorio
Biblioteca Digital (UBA-FCEN)
Institución
Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
OAI Identificador
paperaa:paper_20418205_v708_n2PART2_pL116_Verdini
Acceder
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oai_identifier_str paperaa:paper_20418205_v708_n2PART2_pL116_Verdini
network_acronym_str BDUBAFCEN
repository_id_str 1896
network_name_str Biblioteca Digital (UBA-FCEN)
spelling A turbulence-driven model for heating and acceleration of the fast wind in coronal holesVerdini, A.Velli, M.Matthaeus, W.H.Oughton, S.Dmitruk, P.MHDSolar windTurbulenceWavesA model is presented for generation of fast solar wind in coronal holes, relying on heating that is dominated by turbulent dissipation of MHD fluctuations transported upward in the solar atmosphere. Scale-separated transport equations include large-scale fields, transverse Alfvénic fluctuations, and a small compressive dissipation due to parallel shears near the transition region. The model accounts for proton temperature, density, wind speed, and fluctuation amplitude as observed in remote sensing and in situ satellite data. © 2010. The American Astronomical Society. All rights reserved..Fil:Dmitruk, P. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.2010info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://hdl.handle.net/20.500.12110/paper_20418205_v708_n2PART2_pL116_VerdiniAstrophys. J. Lett. 2010;708(2 PART 2):L116-L120reponame:Biblioteca Digital (UBA-FCEN)instname:Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturalesinstacron:UBA-FCENenginfo:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by/2.5/ar2025-09-29T13:43:03Zpaperaa:paper_20418205_v708_n2PART2_pL116_VerdiniInstitucionalhttps://digital.bl.fcen.uba.ar/Universidad públicaNo correspondehttps://digital.bl.fcen.uba.ar/cgi-bin/oaiserver.cgiana@bl.fcen.uba.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:18962025-09-29 13:43:04.321Biblioteca Digital (UBA-FCEN) - Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturalesfalse
dc.title.none.fl_str_mv A turbulence-driven model for heating and acceleration of the fast wind in coronal holes
title A turbulence-driven model for heating and acceleration of the fast wind in coronal holes
spellingShingle A turbulence-driven model for heating and acceleration of the fast wind in coronal holes
Verdini, A.
MHD
Solar wind
Turbulence
Waves
title_short A turbulence-driven model for heating and acceleration of the fast wind in coronal holes
title_full A turbulence-driven model for heating and acceleration of the fast wind in coronal holes
title_fullStr A turbulence-driven model for heating and acceleration of the fast wind in coronal holes
title_full_unstemmed A turbulence-driven model for heating and acceleration of the fast wind in coronal holes
title_sort A turbulence-driven model for heating and acceleration of the fast wind in coronal holes
dc.creator.none.fl_str_mv Verdini, A.
Velli, M.
Matthaeus, W.H.
Oughton, S.
Dmitruk, P.
author Verdini, A.
author_facet Verdini, A.
Velli, M.
Matthaeus, W.H.
Oughton, S.
Dmitruk, P.
author_role author
author2 Velli, M.
Matthaeus, W.H.
Oughton, S.
Dmitruk, P.
author2_role author
author
author
author
dc.subject.none.fl_str_mv MHD
Solar wind
Turbulence
Waves
topic MHD
Solar wind
Turbulence
Waves
dc.description.none.fl_txt_mv A model is presented for generation of fast solar wind in coronal holes, relying on heating that is dominated by turbulent dissipation of MHD fluctuations transported upward in the solar atmosphere. Scale-separated transport equations include large-scale fields, transverse Alfvénic fluctuations, and a small compressive dissipation due to parallel shears near the transition region. The model accounts for proton temperature, density, wind speed, and fluctuation amplitude as observed in remote sensing and in situ satellite data. © 2010. The American Astronomical Society. All rights reserved..
Fil:Dmitruk, P. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.
description A model is presented for generation of fast solar wind in coronal holes, relying on heating that is dominated by turbulent dissipation of MHD fluctuations transported upward in the solar atmosphere. Scale-separated transport equations include large-scale fields, transverse Alfvénic fluctuations, and a small compressive dissipation due to parallel shears near the transition region. The model accounts for proton temperature, density, wind speed, and fluctuation amplitude as observed in remote sensing and in situ satellite data. © 2010. The American Astronomical Society. All rights reserved..
publishDate 2010
dc.date.none.fl_str_mv 2010
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/20.500.12110/paper_20418205_v708_n2PART2_pL116_Verdini
url http://hdl.handle.net/20.500.12110/paper_20418205_v708_n2PART2_pL116_Verdini
dc.language.none.fl_str_mv eng
language eng
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by/2.5/ar
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by/2.5/ar
dc.format.none.fl_str_mv application/pdf
dc.source.none.fl_str_mv Astrophys. J. Lett. 2010;708(2 PART 2):L116-L120
reponame:Biblioteca Digital (UBA-FCEN)
instname:Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
instacron:UBA-FCEN
reponame_str Biblioteca Digital (UBA-FCEN)
collection Biblioteca Digital (UBA-FCEN)
instname_str Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
instacron_str UBA-FCEN
institution UBA-FCEN
repository.name.fl_str_mv Biblioteca Digital (UBA-FCEN) - Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
repository.mail.fl_str_mv ana@bl.fcen.uba.ar
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score 13.070432

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