Turbulent heating of coronal active regions

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Magnetohydrodynamic turbulence has been proposed as a mechanism for the heating of coronal active regions, and has therefore been actively investigated in recent years. According to this scenario, a turbulent regime is driven by footpoint motions. The energy being pumped this way into active region...

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Autores principales:	Gómez, D.O., Dmitruk, P.
Formato:	Artículo publishedVersion
Lenguaje:	Inglés
Publicado:	2007
Materias:	Coronal heating Mhd turbulence Nanoflares Solar corona
Acceso en línea:	http://hdl.handle.net/20.500.12110/paper_17439213_v3_nS247_p269_Gomez
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	paperaa:paper_17439213_v3_nS247_p269_Gomez
record_format	dspace
spelling	paperaa:paper_17439213_v3_nS247_p269_Gomez2023-06-12T16:51:12Z Turbulent heating of coronal active regions Proc. Int. Astron. Union 2007;3(S247):269-278 Gómez, D.O. Dmitruk, P. Coronal heating Mhd turbulence Nanoflares Solar corona Magnetohydrodynamic turbulence has been proposed as a mechanism for the heating of coronal active regions, and has therefore been actively investigated in recent years. According to this scenario, a turbulent regime is driven by footpoint motions. The energy being pumped this way into active region loops, is efficiently transferred to small scales due to a direct energy cascade. The ensuing generation of fine scale structures, which is a natural outcome of turbulent regimes, helps to enhance the dissipation of either waves or DC currents. We present an updated overview of recent results on turbulent coronal heating. To illustrate this theoretical scenario, we simulate the internal dynamics of a coronal loop within the reduced MHD approximation. The application of a stationary velocity field at the photospheric boundary leads to a turbulent stationary regime after several photospheric turnover times. This regime is characterized by a broadband power spectrum and energy dissipation rate levels compatible with the heating requirements of active region loops. Also, the energy dissipation rate displays a complex superposition of impulsive events, which we associate to the so-called nanoflares. A statistical analysis yields a power law distribution as a function of their energies, which is consistent with those obtained from observations. We also study the distributions of peak dissipation rate and duration of these events. © 2008 International Astronomical Union. Fil:Gómez, D.O. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Dmitruk, P. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. 2007 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_v3_nS247_p269_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	Coronal heating Mhd turbulence Nanoflares Solar corona
spellingShingle	Coronal heating Mhd turbulence Nanoflares Solar corona Gómez, D.O. Dmitruk, P. Turbulent heating of coronal active regions
topic_facet	Coronal heating Mhd turbulence Nanoflares Solar corona
description	Magnetohydrodynamic turbulence has been proposed as a mechanism for the heating of coronal active regions, and has therefore been actively investigated in recent years. According to this scenario, a turbulent regime is driven by footpoint motions. The energy being pumped this way into active region loops, is efficiently transferred to small scales due to a direct energy cascade. The ensuing generation of fine scale structures, which is a natural outcome of turbulent regimes, helps to enhance the dissipation of either waves or DC currents. We present an updated overview of recent results on turbulent coronal heating. To illustrate this theoretical scenario, we simulate the internal dynamics of a coronal loop within the reduced MHD approximation. The application of a stationary velocity field at the photospheric boundary leads to a turbulent stationary regime after several photospheric turnover times. This regime is characterized by a broadband power spectrum and energy dissipation rate levels compatible with the heating requirements of active region loops. Also, the energy dissipation rate displays a complex superposition of impulsive events, which we associate to the so-called nanoflares. A statistical analysis yields a power law distribution as a function of their energies, which is consistent with those obtained from observations. We also study the distributions of peak dissipation rate and duration of these events. © 2008 International Astronomical Union.
format	Artículo Artículo publishedVersion
author	Gómez, D.O. Dmitruk, P.
author_facet	Gómez, D.O. Dmitruk, P.
author_sort	Gómez, D.O.
title	Turbulent heating of coronal active regions
title_short	Turbulent heating of coronal active regions
title_full	Turbulent heating of coronal active regions
title_fullStr	Turbulent heating of coronal active regions
title_full_unstemmed	Turbulent heating of coronal active regions
title_sort	turbulent heating of coronal active regions
publishDate	2007
url	http://hdl.handle.net/20.500.12110/paper_17439213_v3_nS247_p269_Gomez
work_keys_str_mv	AT gomezdo turbulentheatingofcoronalactiveregions AT dmitrukp turbulentheatingofcoronalactiveregions
_version_	1769810047550881792

Turbulent heating of coronal active regions

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