Heating of coronal active regions

Mostrar todas las versiones(3)

Recent observations of coronal loops in solar active regions show that their heating must be a truly dynamic process. Even though it seems clear that the energy source is the magnetic field that confines the coronal plasma, the details of how it dissipates are still a matter of debate. In this prese...

Descripción completa

Guardado en:
Detalles Bibliográficos
Autor principal: Gómez, D.O.
Formato: Artículo publishedVersion
Lenguaje:Inglés
Publicado: 2010
Materias:
Magnetic fiels
MHD
Sun: corona
Sun: X-rays
Turbulence
Acceso en línea:http://hdl.handle.net/20.500.12110/paper_17439213_v6_nS273_p44_Gomez
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paperaa:paper_17439213_v6_nS273_p44_Gomez
record_format dspace
spelling paperaa:paper_17439213_v6_nS273_p44_Gomez2023-06-12T16:51:13Z Heating of coronal active regions Proc. Int. Astron. Union 2010;6(S273):44-50 Gómez, D.O. Magnetic fiels MHD Sun: corona Sun: X-rays Turbulence Recent observations of coronal loops in solar active regions show that their heating must be a truly dynamic process. Even though it seems clear that the energy source is the magnetic field that confines the coronal plasma, the details of how it dissipates are still a matter of debate. In this presentation we review the theoretical models of coronal heating, which have been traditionally clasified as DC or AC depending on the electrodynamic response of the loops to the photospheric driving motions. Also, we show results from numerical simulations of the internal dynamics of coronal loops within the framework of the reduced MHD approximation. These simulations indicate that the application of a stationary velocity field at the photospheric boundary leads to a turbulent stationary regime after several photospheric turnover times. Once this turbulent regime is set, both DC and AC stresses dissipate at faster rates as a result of a direct energy cascade. © International Astronomical Union 2011. Fil:Gómez, D.O. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. 2010 info:eu-repo/semantics/article info:ar-repo/semantics/artículo info:eu-repo/semantics/publishedVersion application/pdf eng info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_17439213_v6_nS273_p44_Gomez
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
language Inglés
orig_language_str_mv eng
topic Magnetic fiels
MHD
Sun: corona
Sun: X-rays
Turbulence
spellingShingle Magnetic fiels
MHD
Sun: corona
Sun: X-rays
Turbulence
Gómez, D.O.
Heating of coronal active regions
topic_facet Magnetic fiels
MHD
Sun: corona
Sun: X-rays
Turbulence
description Recent observations of coronal loops in solar active regions show that their heating must be a truly dynamic process. Even though it seems clear that the energy source is the magnetic field that confines the coronal plasma, the details of how it dissipates are still a matter of debate. In this presentation we review the theoretical models of coronal heating, which have been traditionally clasified as DC or AC depending on the electrodynamic response of the loops to the photospheric driving motions. Also, we show results from numerical simulations of the internal dynamics of coronal loops within the framework of the reduced MHD approximation. These simulations indicate that the application of a stationary velocity field at the photospheric boundary leads to a turbulent stationary regime after several photospheric turnover times. Once this turbulent regime is set, both DC and AC stresses dissipate at faster rates as a result of a direct energy cascade. © International Astronomical Union 2011.
format Artículo
Artículo
publishedVersion
author Gómez, D.O.
author_facet Gómez, D.O.
author_sort Gómez, D.O.
title Heating of coronal active regions
title_short Heating of coronal active regions
title_full Heating of coronal active regions
title_fullStr Heating of coronal active regions
title_full_unstemmed Heating of coronal active regions
title_sort heating of coronal active regions
publishDate 2010
url http://hdl.handle.net/20.500.12110/paper_17439213_v6_nS273_p44_Gomez
work_keys_str_mv AT gomezdo heatingofcoronalactiveregions
_version_ 1769810352815472640

Ejemplares similares