The long-term evolution of AR 7978: Testing coronal heating models

We derive the dependence of the mean coronal heating rate on the magnetic flux density. Our results are based on a previous study of the plasma parameters and the magnetic flux density (B̄) in the active region NOAA 7978 from its birth to its decay, throughout five solar rotations using the Solar an...

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Autores principales: Démoulin, P., Van Driel-Gesztelyi, L., Mandrini, C.H., Klimchuk, J.A., Harra, L.
Formato: JOUR
Materias:
Magnetic fields
Sun: corona
Sun: magnetic fields
Sun: X-rays, gamma rays
Acceso en línea:http://hdl.handle.net/20.500.12110/paper_0004637X_v586_n1I_p592_Demoulin
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
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spelling todo:paper_0004637X_v586_n1I_p592_Demoulin2023-10-03T14:01:53Z The long-term evolution of AR 7978: Testing coronal heating models Démoulin, P. Van Driel-Gesztelyi, L. Mandrini, C.H. Klimchuk, J.A. Harra, L. Magnetic fields Sun: corona Sun: magnetic fields Sun: X-rays, gamma rays We derive the dependence of the mean coronal heating rate on the magnetic flux density. Our results are based on a previous study of the plasma parameters and the magnetic flux density (B̄) in the active region NOAA 7978 from its birth to its decay, throughout five solar rotations using the Solar and Heliospheric Observatory Michelson Doppler Imager, Yohkoh Soft X-Ray Telescope (SXT), and Yohkoh Bragg Crystal Spectrometer (BCS). We use the scaling laws of coronal loops in thermal equilibrium to derive four observational estimates of the scaling of the coronal heating with B̄ (two from SXT and two from BCS observations). These results are used to test the validity of coronal heating models. We find that models based on the dissipation of stressed, current-carrying magnetic fields are in better agreement with the observations than models that attribute coronal heating to the dissipation of MHD waves injected at the base of the corona. This confirms, with smaller error bars, previous results obtained for individual coronal loops, as well as for the global coronal emission of the Sun and cool stars. Taking into account that the photospheric field is concentrated in thin magnetic flux tubes, both SXT and BCS data are in best agreement with models invoking a stochastic buildup of energy, current layers, and MHD turbulence. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_0004637X_v586_n1I_p592_Demoulin
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Magnetic fields
Sun: corona
Sun: magnetic fields
Sun: X-rays, gamma rays
spellingShingle Magnetic fields
Sun: corona
Sun: magnetic fields
Sun: X-rays, gamma rays
Démoulin, P.
Van Driel-Gesztelyi, L.
Mandrini, C.H.
Klimchuk, J.A.
Harra, L.
The long-term evolution of AR 7978: Testing coronal heating models
topic_facet Magnetic fields
Sun: corona
Sun: magnetic fields
Sun: X-rays, gamma rays
description We derive the dependence of the mean coronal heating rate on the magnetic flux density. Our results are based on a previous study of the plasma parameters and the magnetic flux density (B̄) in the active region NOAA 7978 from its birth to its decay, throughout five solar rotations using the Solar and Heliospheric Observatory Michelson Doppler Imager, Yohkoh Soft X-Ray Telescope (SXT), and Yohkoh Bragg Crystal Spectrometer (BCS). We use the scaling laws of coronal loops in thermal equilibrium to derive four observational estimates of the scaling of the coronal heating with B̄ (two from SXT and two from BCS observations). These results are used to test the validity of coronal heating models. We find that models based on the dissipation of stressed, current-carrying magnetic fields are in better agreement with the observations than models that attribute coronal heating to the dissipation of MHD waves injected at the base of the corona. This confirms, with smaller error bars, previous results obtained for individual coronal loops, as well as for the global coronal emission of the Sun and cool stars. Taking into account that the photospheric field is concentrated in thin magnetic flux tubes, both SXT and BCS data are in best agreement with models invoking a stochastic buildup of energy, current layers, and MHD turbulence.
format JOUR
author Démoulin, P.
Van Driel-Gesztelyi, L.
Mandrini, C.H.
Klimchuk, J.A.
Harra, L.
author_facet Démoulin, P.
Van Driel-Gesztelyi, L.
Mandrini, C.H.
Klimchuk, J.A.
Harra, L.
author_sort Démoulin, P.
title The long-term evolution of AR 7978: Testing coronal heating models
title_short The long-term evolution of AR 7978: Testing coronal heating models
title_full The long-term evolution of AR 7978: Testing coronal heating models
title_fullStr The long-term evolution of AR 7978: Testing coronal heating models
title_full_unstemmed The long-term evolution of AR 7978: Testing coronal heating models
title_sort long-term evolution of ar 7978: testing coronal heating models
url http://hdl.handle.net/20.500.12110/paper_0004637X_v586_n1I_p592_Demoulin
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