Origin of the Submillimeter Radio Emission During the Time-Extended Phase of a Solar Flare

Autores
Trottet, G.; Raulin, J. P.; Castro, C. G. Giménez de; Luthi, T; Caspi, A.; Mandrini, Cristina Hemilse; Luoni, Maria Luisa; Kaufmann, Pierre
Año de publicación
2011
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
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.
Fil: Trottet, G.. Universidade Presbiteriana Mackenzie; Brasil
Fil: Raulin, J. P.. Universidade Presbiteriana Mackenzie; Brasil
Fil: Castro, C. G. Giménez de. Universidade Presbiteriana Mackenzie; Brasil
Fil: Luthi, T. Hexagon Metrology; Suiza
Fil: Caspi, A.. University of California; Estados Unidos
Fil: Mandrini, Cristina Hemilse. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Luoni, Maria Luisa. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Kaufmann, Pierre. Universidade Presbiteriana Mackenzie; Brasil
Materia
Radio Bursts,Association with Flares
Radio Bursts, Microwave
X-Ray Bursts, Association with Flares
Flares, Relation to Magnetic Field
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/20028
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/20028
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Origin of the Submillimeter Radio Emission During the Time-Extended Phase of a Solar FlareTrottet, G.Raulin, J. P.Castro, C. G. Giménez deLuthi, TCaspi, A.Mandrini, Cristina HemilseLuoni, Maria LuisaKaufmann, PierreRadio Bursts,Association with FlaresRadio Bursts, MicrowaveX-Ray Bursts, Association with FlaresFlares, Relation to Magnetic Fieldhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Solar 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 10<sup>4</sup> 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.Fil: Trottet, G.. Universidade Presbiteriana Mackenzie; BrasilFil: Raulin, J. P.. Universidade Presbiteriana Mackenzie; BrasilFil: Castro, C. G. Giménez de. Universidade Presbiteriana Mackenzie; BrasilFil: Luthi, T. Hexagon Metrology; SuizaFil: Caspi, A.. University of California; Estados UnidosFil: Mandrini, Cristina Hemilse. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Luoni, Maria Luisa. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Kaufmann, Pierre. Universidade Presbiteriana Mackenzie; BrasilSpringer2011-11info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/20028Trottet, G.; Raulin, J. P.; Castro, C. G. Giménez de; Luthi, T; Caspi, A.; et al.; Origin of the Submillimeter Radio Emission During the Time-Extended Phase of a Solar Flare; Springer; Solar Physics; 273; 2; 11-2011; 339-3610038-0938CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1109.5729info:eu-repo/semantics/altIdentifier/url/https://link.springer.com/article/10.1007/s11207-011-9875-6info:eu-repo/semantics/altIdentifier/doi/10.1007/s11207-011-9875-6info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:59:41Zoai:ri.conicet.gov.ar:11336/20028instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 09:59:41.749CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Origin of the Submillimeter Radio Emission During the Time-Extended Phase of a Solar Flare
title Origin of the Submillimeter Radio Emission During the Time-Extended Phase of a Solar Flare
spellingShingle Origin of the Submillimeter Radio Emission During the Time-Extended Phase of a Solar Flare
Trottet, G.
Radio Bursts,Association with Flares
Radio Bursts, Microwave
X-Ray Bursts, Association with Flares
Flares, Relation to Magnetic Field
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
dc.creator.none.fl_str_mv Trottet, G.
Raulin, J. P.
Castro, C. G. Giménez de
Luthi, T
Caspi, A.
Mandrini, Cristina Hemilse
Luoni, Maria Luisa
Kaufmann, Pierre
author Trottet, G.
author_facet Trottet, G.
Raulin, J. P.
Castro, C. G. Giménez de
Luthi, T
Caspi, A.
Mandrini, Cristina Hemilse
Luoni, Maria Luisa
Kaufmann, Pierre
author_role author
author2 Raulin, J. P.
Castro, C. G. Giménez de
Luthi, T
Caspi, A.
Mandrini, Cristina Hemilse
Luoni, Maria Luisa
Kaufmann, Pierre
author2_role author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Radio Bursts,Association with Flares
Radio Bursts, Microwave
X-Ray Bursts, Association with Flares
Flares, Relation to Magnetic Field
topic Radio Bursts,Association with Flares
Radio Bursts, Microwave
X-Ray Bursts, Association with Flares
Flares, Relation to Magnetic Field
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv 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 10<sup>4</sup> 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.
Fil: Trottet, G.. Universidade Presbiteriana Mackenzie; Brasil
Fil: Raulin, J. P.. Universidade Presbiteriana Mackenzie; Brasil
Fil: Castro, C. G. Giménez de. Universidade Presbiteriana Mackenzie; Brasil
Fil: Luthi, T. Hexagon Metrology; Suiza
Fil: Caspi, A.. University of California; Estados Unidos
Fil: Mandrini, Cristina Hemilse. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Luoni, Maria Luisa. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Kaufmann, Pierre. Universidade Presbiteriana Mackenzie; Brasil
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 10<sup>4</sup> 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.
publishDate 2011
dc.date.none.fl_str_mv 2011-11
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/20028
Trottet, G.; Raulin, J. P.; Castro, C. G. Giménez de; Luthi, T; Caspi, A.; et al.; Origin of the Submillimeter Radio Emission During the Time-Extended Phase of a Solar Flare; Springer; Solar Physics; 273; 2; 11-2011; 339-361
0038-0938
CONICET Digital
CONICET
url http://hdl.handle.net/11336/20028
identifier_str_mv Trottet, G.; Raulin, J. P.; Castro, C. G. Giménez de; Luthi, T; Caspi, A.; et al.; Origin of the Submillimeter Radio Emission During the Time-Extended Phase of a Solar Flare; Springer; Solar Physics; 273; 2; 11-2011; 339-361
0038-0938
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1109.5729
info:eu-repo/semantics/altIdentifier/url/https://link.springer.com/article/10.1007/s11207-011-9875-6
info:eu-repo/semantics/altIdentifier/doi/10.1007/s11207-011-9875-6
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
application/pdf
application/pdf
dc.publisher.none.fl_str_mv Springer
publisher.none.fl_str_mv Springer
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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score 13.070432

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