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-lastin...

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Autores principales: Giménez de Castro, Carlos Guillermo, Mandrini, Cristina Hemilse, Luoni, Maria Luisa
Publicado: 2011
Materias:
Chromosphere, active
Flares, relation to magnetic field
Radio bursts, association with flares
Radio bursts, microwave
X-ray bursts, association with flares
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00380938_v273_n2_p339_Trottet
http://hdl.handle.net/20.500.12110/paper_00380938_v273_n2_p339_Trottet
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Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
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spelling paper:paper_00380938_v273_n2_p339_Trottet2023-06-08T15:02:46Z Origin of the Submillimeter Radio Emission During the Time-Extended Phase of a Solar Flare Giménez de Castro, Carlos Guillermo Mandrini, Cristina Hemilse Luoni, Maria Luisa Chromosphere, active Flares, relation to magnetic field Radio bursts, association with flares Radio bursts, microwave X-ray bursts, association with flares 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. © 2011 Springer Science+Business Media B.V. Fil:Giménez de Castro, G. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Mandrini, C.H. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Luoni, M.L. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. 2011 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00380938_v273_n2_p339_Trottet http://hdl.handle.net/20.500.12110/paper_00380938_v273_n2_p339_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 Chromosphere, active
Flares, relation to magnetic field
Radio bursts, association with flares
Radio bursts, microwave
X-ray bursts, association with flares
spellingShingle Chromosphere, active
Flares, relation to magnetic field
Radio bursts, association with flares
Radio bursts, microwave
X-ray bursts, association with flares
Giménez de Castro, Carlos Guillermo
Mandrini, Cristina Hemilse
Luoni, Maria Luisa
Origin of the Submillimeter Radio Emission During the Time-Extended Phase of a Solar Flare
topic_facet Chromosphere, active
Flares, relation to magnetic field
Radio bursts, association with flares
Radio bursts, microwave
X-ray bursts, association with flares
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. © 2011 Springer Science+Business Media B.V.
author Giménez de Castro, Carlos Guillermo
Mandrini, Cristina Hemilse
Luoni, Maria Luisa
author_facet Giménez de Castro, Carlos Guillermo
Mandrini, Cristina Hemilse
Luoni, Maria Luisa
author_sort Giménez de Castro, Carlos Guillermo
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 2011
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00380938_v273_n2_p339_Trottet
http://hdl.handle.net/20.500.12110/paper_00380938_v273_n2_p339_Trottet
work_keys_str_mv AT gimenezdecastrocarlosguillermo originofthesubmillimeterradioemissionduringthetimeextendedphaseofasolarflare
AT mandrinicristinahemilse originofthesubmillimeterradioemissionduringthetimeextendedphaseofasolarflare
AT luonimarialuisa originofthesubmillimeterradioemissionduringthetimeextendedphaseofasolarflare
_version_ 1768542978987524096

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