Submillimeter and X-ray observations of an X class flare

Autores
Gimenez de Castro, Carlos Guillermo; Trottet, G.; Silva Valio, Adriana; Krucker, Sam; Costa, Joaquim; Kaufmann, Pierre; Correia, Emilia; Levato, Orlando Hugo
Año de publicación
2009
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The GOES X1.5 class flare that occurred on August 30, 2002 at 1327:30 UT is one of the few events detected so far at submillimeter wavelengths. We present a detailed analysis of this flare combining radio observations from 1.5 to 212 GHz (an upper limit of the flux is also provided at 405 GHz) and X-ray. Although the observations of radio emission up to 212 GHz indicates that relativistic electrons with energies of a few MeV were accelerated, no significant hard X-ray emission was detected by RHESSI above ∼250 keV. Images at 12-20 and 50-100 keV reveal a very compact, but resolved, source of about ∼10" ×10". EUV TRACE images show a multi-kernel structure suggesting a complex (multipolar) magnetic topology. During the peak time the radio spectrum shows an extended flatness from ∼7 to 35 GHz. Modeling the optically thin part of the radio spectrum as gyrosynchrotron emission we obtained the electron spectrum (spectral index d, instantaneous number of emitting electrons). It is shown that in order to keep the expected X-ray emission from the same emitting electrons below the RHESSI background at 250 keV, a magnetic field above 500 G is necessary. On the other hand, the electron spectrum deduced from radio observations =50 GHz is harder than that deduced from 70-250 keV X-ray data, meaning that there must exist a breaking energy around a few hundred keV. During the decay of the impulsive phase, a hardening of the X-ray spectrum is observed which is interpreted as a hardening of the electron distribution spectrum produced by the diffusion due to Coulomb collisions of the trapped electrons in a medium with an electron density of ne ∼ 3-5 × 1010 cm-3. © 2009 ESO.
Fil: Gimenez de Castro, Carlos Guillermo. Universidad Presbiteriana Mackenzie. Centro de Radiotronomia y Astrofisica; Brasil
Fil: Trottet, G.. Observatorio de Paris; Francia
Fil: Silva Valio, Adriana. Universidad Presbiteriana Mackenzie. Centro de Radiotronomia y Astrofisica; Brasil
Fil: Krucker, Sam. University of California; Estados Unidos
Fil: Costa, Joaquim. Instituto Nacional de Pesquisas Espaciais; Brasil
Fil: Kaufmann, Pierre. Universidade Estadual de Campinas; Brasil
Fil: Correia, Emilia. Universidad Presbiteriana Mackenzie; Brasil
Fil: Levato, Orlando Hugo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina
Materia
SUN: ACTIVITY
FLARES
PARTICLE EMISSION
RADIO RADIATION
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:11336/171583
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/171583
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Submillimeter and X-ray observations of an X class flareGimenez de Castro, Carlos GuillermoTrottet, G.Silva Valio, AdrianaKrucker, SamCosta, JoaquimKaufmann, PierreCorreia, EmiliaLevato, Orlando HugoSUN: ACTIVITYFLARESPARTICLE EMISSIONRADIO RADIATIONhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The GOES X1.5 class flare that occurred on August 30, 2002 at 1327:30 UT is one of the few events detected so far at submillimeter wavelengths. We present a detailed analysis of this flare combining radio observations from 1.5 to 212 GHz (an upper limit of the flux is also provided at 405 GHz) and X-ray. Although the observations of radio emission up to 212 GHz indicates that relativistic electrons with energies of a few MeV were accelerated, no significant hard X-ray emission was detected by RHESSI above ∼250 keV. Images at 12-20 and 50-100 keV reveal a very compact, but resolved, source of about ∼10" ×10". EUV TRACE images show a multi-kernel structure suggesting a complex (multipolar) magnetic topology. During the peak time the radio spectrum shows an extended flatness from ∼7 to 35 GHz. Modeling the optically thin part of the radio spectrum as gyrosynchrotron emission we obtained the electron spectrum (spectral index d, instantaneous number of emitting electrons). It is shown that in order to keep the expected X-ray emission from the same emitting electrons below the RHESSI background at 250 keV, a magnetic field above 500 G is necessary. On the other hand, the electron spectrum deduced from radio observations =50 GHz is harder than that deduced from 70-250 keV X-ray data, meaning that there must exist a breaking energy around a few hundred keV. During the decay of the impulsive phase, a hardening of the X-ray spectrum is observed which is interpreted as a hardening of the electron distribution spectrum produced by the diffusion due to Coulomb collisions of the trapped electrons in a medium with an electron density of ne ∼ 3-5 × 1010 cm-3. © 2009 ESO.Fil: Gimenez de Castro, Carlos Guillermo. Universidad Presbiteriana Mackenzie. Centro de Radiotronomia y Astrofisica; BrasilFil: Trottet, G.. Observatorio de Paris; FranciaFil: Silva Valio, Adriana. Universidad Presbiteriana Mackenzie. Centro de Radiotronomia y Astrofisica; BrasilFil: Krucker, Sam. University of California; Estados UnidosFil: Costa, Joaquim. Instituto Nacional de Pesquisas Espaciais; BrasilFil: Kaufmann, Pierre. Universidade Estadual de Campinas; BrasilFil: Correia, Emilia. Universidad Presbiteriana Mackenzie; BrasilFil: Levato, Orlando Hugo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaEDP Sciences2009-11info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/171583Gimenez de Castro, Carlos Guillermo; Trottet, G.; Silva Valio, Adriana; Krucker, Sam; Costa, Joaquim; et al.; Submillimeter and X-ray observations of an X class flare; EDP Sciences; Astronomy and Astrophysics; 507; 1; 11-2009; 433-4390004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/200912028info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2009/43/aa12028-09/aa12028-09.htmlinfo:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/0908.2339v1info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:51:35Zoai:ri.conicet.gov.ar:11336/171583instacron: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:34982025-10-22 11:51:35.84CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Submillimeter and X-ray observations of an X class flare
title Submillimeter and X-ray observations of an X class flare
spellingShingle Submillimeter and X-ray observations of an X class flare
Gimenez de Castro, Carlos Guillermo
SUN: ACTIVITY
FLARES
PARTICLE EMISSION
RADIO RADIATION
title_short Submillimeter and X-ray observations of an X class flare
title_full Submillimeter and X-ray observations of an X class flare
title_fullStr Submillimeter and X-ray observations of an X class flare
title_full_unstemmed Submillimeter and X-ray observations of an X class flare
title_sort Submillimeter and X-ray observations of an X class flare
dc.creator.none.fl_str_mv Gimenez de Castro, Carlos Guillermo
Trottet, G.
Silva Valio, Adriana
Krucker, Sam
Costa, Joaquim
Kaufmann, Pierre
Correia, Emilia
Levato, Orlando Hugo
author Gimenez de Castro, Carlos Guillermo
author_facet Gimenez de Castro, Carlos Guillermo
Trottet, G.
Silva Valio, Adriana
Krucker, Sam
Costa, Joaquim
Kaufmann, Pierre
Correia, Emilia
Levato, Orlando Hugo
author_role author
author2 Trottet, G.
Silva Valio, Adriana
Krucker, Sam
Costa, Joaquim
Kaufmann, Pierre
Correia, Emilia
Levato, Orlando Hugo
author2_role author
author
author
author
author
author
author
dc.subject.none.fl_str_mv SUN: ACTIVITY
FLARES
PARTICLE EMISSION
RADIO RADIATION
topic SUN: ACTIVITY
FLARES
PARTICLE EMISSION
RADIO RADIATION
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv The GOES X1.5 class flare that occurred on August 30, 2002 at 1327:30 UT is one of the few events detected so far at submillimeter wavelengths. We present a detailed analysis of this flare combining radio observations from 1.5 to 212 GHz (an upper limit of the flux is also provided at 405 GHz) and X-ray. Although the observations of radio emission up to 212 GHz indicates that relativistic electrons with energies of a few MeV were accelerated, no significant hard X-ray emission was detected by RHESSI above ∼250 keV. Images at 12-20 and 50-100 keV reveal a very compact, but resolved, source of about ∼10" ×10". EUV TRACE images show a multi-kernel structure suggesting a complex (multipolar) magnetic topology. During the peak time the radio spectrum shows an extended flatness from ∼7 to 35 GHz. Modeling the optically thin part of the radio spectrum as gyrosynchrotron emission we obtained the electron spectrum (spectral index d, instantaneous number of emitting electrons). It is shown that in order to keep the expected X-ray emission from the same emitting electrons below the RHESSI background at 250 keV, a magnetic field above 500 G is necessary. On the other hand, the electron spectrum deduced from radio observations =50 GHz is harder than that deduced from 70-250 keV X-ray data, meaning that there must exist a breaking energy around a few hundred keV. During the decay of the impulsive phase, a hardening of the X-ray spectrum is observed which is interpreted as a hardening of the electron distribution spectrum produced by the diffusion due to Coulomb collisions of the trapped electrons in a medium with an electron density of ne ∼ 3-5 × 1010 cm-3. © 2009 ESO.
Fil: Gimenez de Castro, Carlos Guillermo. Universidad Presbiteriana Mackenzie. Centro de Radiotronomia y Astrofisica; Brasil
Fil: Trottet, G.. Observatorio de Paris; Francia
Fil: Silva Valio, Adriana. Universidad Presbiteriana Mackenzie. Centro de Radiotronomia y Astrofisica; Brasil
Fil: Krucker, Sam. University of California; Estados Unidos
Fil: Costa, Joaquim. Instituto Nacional de Pesquisas Espaciais; Brasil
Fil: Kaufmann, Pierre. Universidade Estadual de Campinas; Brasil
Fil: Correia, Emilia. Universidad Presbiteriana Mackenzie; Brasil
Fil: Levato, Orlando Hugo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina
description The GOES X1.5 class flare that occurred on August 30, 2002 at 1327:30 UT is one of the few events detected so far at submillimeter wavelengths. We present a detailed analysis of this flare combining radio observations from 1.5 to 212 GHz (an upper limit of the flux is also provided at 405 GHz) and X-ray. Although the observations of radio emission up to 212 GHz indicates that relativistic electrons with energies of a few MeV were accelerated, no significant hard X-ray emission was detected by RHESSI above ∼250 keV. Images at 12-20 and 50-100 keV reveal a very compact, but resolved, source of about ∼10" ×10". EUV TRACE images show a multi-kernel structure suggesting a complex (multipolar) magnetic topology. During the peak time the radio spectrum shows an extended flatness from ∼7 to 35 GHz. Modeling the optically thin part of the radio spectrum as gyrosynchrotron emission we obtained the electron spectrum (spectral index d, instantaneous number of emitting electrons). It is shown that in order to keep the expected X-ray emission from the same emitting electrons below the RHESSI background at 250 keV, a magnetic field above 500 G is necessary. On the other hand, the electron spectrum deduced from radio observations =50 GHz is harder than that deduced from 70-250 keV X-ray data, meaning that there must exist a breaking energy around a few hundred keV. During the decay of the impulsive phase, a hardening of the X-ray spectrum is observed which is interpreted as a hardening of the electron distribution spectrum produced by the diffusion due to Coulomb collisions of the trapped electrons in a medium with an electron density of ne ∼ 3-5 × 1010 cm-3. © 2009 ESO.
publishDate 2009
dc.date.none.fl_str_mv 2009-11
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/11336/171583
Gimenez de Castro, Carlos Guillermo; Trottet, G.; Silva Valio, Adriana; Krucker, Sam; Costa, Joaquim; et al.; Submillimeter and X-ray observations of an X class flare; EDP Sciences; Astronomy and Astrophysics; 507; 1; 11-2009; 433-439
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/171583
identifier_str_mv Gimenez de Castro, Carlos Guillermo; Trottet, G.; Silva Valio, Adriana; Krucker, Sam; Costa, Joaquim; et al.; Submillimeter and X-ray observations of an X class flare; EDP Sciences; Astronomy and Astrophysics; 507; 1; 11-2009; 433-439
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/200912028
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2009/43/aa12028-09/aa12028-09.html
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/0908.2339v1
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
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
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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