Turbulent heating of coronal active regions

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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Detalles Bibliográficos
Autores principales:	Gomez, Daniel Osvaldo, Dmitruk, Pablo Ariel
Publicado:	2007
Materias:	Coronal heating Mhd turbulence Nanoflares Solar corona
Acceso en línea:	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_17439213_v3_nS247_p269_Gomez 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	paper:paper_17439213_v3_nS247_p269_Gomez
record_format	dspace
spelling	paper:paper_17439213_v3_nS247_p269_Gomez2023-06-08T16:27:59Z Turbulent heating of coronal active regions Gomez, Daniel Osvaldo Dmitruk, Pablo Ariel 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 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_17439213_v3_nS247_p269_Gomez 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)
topic	Coronal heating Mhd turbulence Nanoflares Solar corona
spellingShingle	Coronal heating Mhd turbulence Nanoflares Solar corona Gomez, Daniel Osvaldo Dmitruk, Pablo Ariel 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.
author	Gomez, Daniel Osvaldo Dmitruk, Pablo Ariel
author_facet	Gomez, Daniel Osvaldo Dmitruk, Pablo Ariel
author_sort	Gomez, Daniel Osvaldo
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	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_17439213_v3_nS247_p269_Gomez http://hdl.handle.net/20.500.12110/paper_17439213_v3_nS247_p269_Gomez
work_keys_str_mv	AT gomezdanielosvaldo turbulentheatingofcoronalactiveregions AT dmitrukpabloariel turbulentheatingofcoronalactiveregions
_version_	1768542906569719808

Turbulent heating of coronal active regions

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