Origin of the submillimeter radio emission during the time-extended phase of a solar flare

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Solar flares observed in the 200∈-∈400 GHz radio domain may exhibit a slowly varying and time-extended component which follows a short (few minutes) impulsive phase and can last for a few tens of minutes to more than one hour. The few examples discussed in the literature indicate that such long-last...

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Autor principal:	Luoni, Maria Luisa
Publicado:	2012
Materias:	active association with flares Chromosphere Flares microwave Radio bursts relation to magnetic field X-ray bursts Energy management Energy resources Microwaves Chromophores
Acceso en línea:	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_97814614_v9781461444039_n_p33_Trottet http://hdl.handle.net/20.500.12110/paper_97814614_v9781461444039_n_p33_Trottet
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	paper:paper_97814614_v9781461444039_n_p33_Trottet
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spelling	paper:paper_97814614_v9781461444039_n_p33_Trottet2023-06-08T16:37:37Z Origin of the submillimeter radio emission during the time-extended phase of a solar flare Luoni, Maria Luisa active association with flares association with flares Chromosphere Flares microwave Radio bursts Radio bursts relation to magnetic field X-ray bursts Energy management Energy resources Microwaves active Chromosphere Flares Radio bursts X-ray bursts Chromophores Solar flares observed in the 200∈-∈400 GHz radio domain may exhibit a slowly varying and time-extended component which follows a short (few minutes) impulsive phase and can last for a few tens of minutes to more than one hour. The few examples discussed in the literature indicate that such long-lasting submillimeter emission is most likely thermal bremsstrahlung. We present a detailed analysis of the time-extended phase of the 27 October 2003 (M6.7) flare, combining 1∈-∈345 GHz total-flux radio measurements with X-ray, EUV, and Hα observations. We find that the time-extended radio emission is, as expected, radiated by thermal bremsstrahlung. Up to 230 GHz, it is entirely produced in the corona by hot and cool materials at 7∈-∈16 MK and 1∈-∈3 MK, respectively. At 345 GHz, there is an additional contribution from chromospheric material at a few 104 K. These results, which may also apply to other millimeter-submillimeter radio events, are not consistent with the expectations from standard semiempirical models of the chromosphere and transition region during flares, which predict observable radio emission from the chromosphere at all frequencies where the corona is transparent. © Springer Science+Business Media New York 2012. All rights are reserved. Fil:Luoni, M.L. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. 2012 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_97814614_v9781461444039_n_p33_Trottet http://hdl.handle.net/20.500.12110/paper_97814614_v9781461444039_n_p33_Trottet
institution	Universidad de Buenos Aires
institution_str	I-28
repository_str	R-134
collection	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic	active association with flares association with flares Chromosphere Flares microwave Radio bursts Radio bursts relation to magnetic field X-ray bursts Energy management Energy resources Microwaves active Chromosphere Flares Radio bursts X-ray bursts Chromophores
spellingShingle	active association with flares association with flares Chromosphere Flares microwave Radio bursts Radio bursts relation to magnetic field X-ray bursts Energy management Energy resources Microwaves active Chromosphere Flares Radio bursts X-ray bursts Chromophores Luoni, Maria Luisa Origin of the submillimeter radio emission during the time-extended phase of a solar flare
topic_facet	active association with flares association with flares Chromosphere Flares microwave Radio bursts Radio bursts relation to magnetic field X-ray bursts Energy management Energy resources Microwaves active Chromosphere Flares Radio bursts X-ray bursts Chromophores
description	Solar flares observed in the 200∈-∈400 GHz radio domain may exhibit a slowly varying and time-extended component which follows a short (few minutes) impulsive phase and can last for a few tens of minutes to more than one hour. The few examples discussed in the literature indicate that such long-lasting submillimeter emission is most likely thermal bremsstrahlung. We present a detailed analysis of the time-extended phase of the 27 October 2003 (M6.7) flare, combining 1∈-∈345 GHz total-flux radio measurements with X-ray, EUV, and Hα observations. We find that the time-extended radio emission is, as expected, radiated by thermal bremsstrahlung. Up to 230 GHz, it is entirely produced in the corona by hot and cool materials at 7∈-∈16 MK and 1∈-∈3 MK, respectively. At 345 GHz, there is an additional contribution from chromospheric material at a few 104 K. These results, which may also apply to other millimeter-submillimeter radio events, are not consistent with the expectations from standard semiempirical models of the chromosphere and transition region during flares, which predict observable radio emission from the chromosphere at all frequencies where the corona is transparent. © Springer Science+Business Media New York 2012. All rights are reserved.
author	Luoni, Maria Luisa
author_facet	Luoni, Maria Luisa
author_sort	Luoni, Maria Luisa
title	Origin of the submillimeter radio emission during the time-extended phase of a solar flare
title_short	Origin of the submillimeter radio emission during the time-extended phase of a solar flare
title_full	Origin of the submillimeter radio emission during the time-extended phase of a solar flare
title_fullStr	Origin of the submillimeter radio emission during the time-extended phase of a solar flare
title_full_unstemmed	Origin of the submillimeter radio emission during the time-extended phase of a solar flare
title_sort	origin of the submillimeter radio emission during the time-extended phase of a solar flare
publishDate	2012
url	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_97814614_v9781461444039_n_p33_Trottet http://hdl.handle.net/20.500.12110/paper_97814614_v9781461444039_n_p33_Trottet
work_keys_str_mv	AT luonimarialuisa originofthesubmillimeterradioemissionduringthetimeextendedphaseofasolarflare
_version_	1768541679635136512

Origin of the submillimeter radio emission during the time-extended phase of a solar flare

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