A magnetic reconnection model for explaining the multi-wavelength emission of the microquasars Cyg X-1 and Cyg X-3

Autores
Khiali, Behrouz; Gouveia Dal Pino, E. M.; del Valle, Maria Victoria
Año de publicación
2015
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Recent studies have indicated that cosmic ray acceleration by a first-order Fermi process in magnetic reconnection current sheets can be efficient enough in the surrounds of compact sources. In this work, we discuss this acceleration mechanism operating in the core region of galactic black hole binaries (or microquasars) and show the conditions under which this can be more efficient than shock acceleration. In addition, we compare the corresponding acceleration rate with the relevant radiative loss rates obtaining the possible energy cut-off of the accelerated particles and also compute the expected spectral energy distribution (SED) for two sources of this class, namely Cygnus X-1 and Cygnus X-3, considering both leptonic and hadronic processes. The derived SEDs are comparable to the observed ones in the low- and high-energy ranges. Our results suggest that hadronic non-thermal emission due to photomeson production may produce the very high energy gamma-rays in these microquasars.
Fil: Khiali, Behrouz. Universidade Do Sao Paulo. Instituto Astronomia, Geofisica E Ciencias Atmosfericas; Brasil
Fil: Gouveia Dal Pino, E. M.. Universidade Do Sao Paulo. Instituto Astronomia, Geofisica E Ciencias Atmosfericas; Brasil
Fil: del Valle, Maria Victoria. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto Argentino de Radioastronomia (i); Argentina
Materia
Microquasars
Cosmic ray acceleration
Non thermal mechanisms
Radiation mechanisms
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:11336/7676
Acceder
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network_name_str CONICET Digital (CONICET)
spelling A magnetic reconnection model for explaining the multi-wavelength emission of the microquasars Cyg X-1 and Cyg X-3Khiali, BehrouzGouveia Dal Pino, E. M.del Valle, Maria VictoriaMicroquasarsCosmic ray accelerationNon thermal mechanismsRadiation mechanismshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Recent studies have indicated that cosmic ray acceleration by a first-order Fermi process in magnetic reconnection current sheets can be efficient enough in the surrounds of compact sources. In this work, we discuss this acceleration mechanism operating in the core region of galactic black hole binaries (or microquasars) and show the conditions under which this can be more efficient than shock acceleration. In addition, we compare the corresponding acceleration rate with the relevant radiative loss rates obtaining the possible energy cut-off of the accelerated particles and also compute the expected spectral energy distribution (SED) for two sources of this class, namely Cygnus X-1 and Cygnus X-3, considering both leptonic and hadronic processes. The derived SEDs are comparable to the observed ones in the low- and high-energy ranges. Our results suggest that hadronic non-thermal emission due to photomeson production may produce the very high energy gamma-rays in these microquasars.Fil: Khiali, Behrouz. Universidade Do Sao Paulo. Instituto Astronomia, Geofisica E Ciencias Atmosfericas; BrasilFil: Gouveia Dal Pino, E. M.. Universidade Do Sao Paulo. Instituto Astronomia, Geofisica E Ciencias Atmosfericas; BrasilFil: del Valle, Maria Victoria. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto Argentino de Radioastronomia (i); ArgentinaOxford University Press2015-02info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/zipapplication/pdfhttp://hdl.handle.net/11336/7676Khiali, Behrouz; Gouveia Dal Pino, E. M.; del Valle, Maria Victoria; A magnetic reconnection model for explaining the multi-wavelength emission of the microquasars Cyg X-1 and Cyg X-3; Oxford University Press; Monthly Notices Of The Royal Astronomical Society; 449; 1; 2-2015; 34-480035-8711enginfo:eu-repo/semantics/altIdentifier/url/http://mnras.oxfordjournals.org/content/449/1/34.abstractinfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stv248info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T14:36:52Zoai:ri.conicet.gov.ar:11336/7676instacron: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:34982025-10-15 14:36:53.004CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv A magnetic reconnection model for explaining the multi-wavelength emission of the microquasars Cyg X-1 and Cyg X-3
title A magnetic reconnection model for explaining the multi-wavelength emission of the microquasars Cyg X-1 and Cyg X-3
spellingShingle A magnetic reconnection model for explaining the multi-wavelength emission of the microquasars Cyg X-1 and Cyg X-3
Khiali, Behrouz
Microquasars
Cosmic ray acceleration
Non thermal mechanisms
Radiation mechanisms
title_short A magnetic reconnection model for explaining the multi-wavelength emission of the microquasars Cyg X-1 and Cyg X-3
title_full A magnetic reconnection model for explaining the multi-wavelength emission of the microquasars Cyg X-1 and Cyg X-3
title_fullStr A magnetic reconnection model for explaining the multi-wavelength emission of the microquasars Cyg X-1 and Cyg X-3
title_full_unstemmed A magnetic reconnection model for explaining the multi-wavelength emission of the microquasars Cyg X-1 and Cyg X-3
title_sort A magnetic reconnection model for explaining the multi-wavelength emission of the microquasars Cyg X-1 and Cyg X-3
dc.creator.none.fl_str_mv Khiali, Behrouz
Gouveia Dal Pino, E. M.
del Valle, Maria Victoria
author Khiali, Behrouz
author_facet Khiali, Behrouz
Gouveia Dal Pino, E. M.
del Valle, Maria Victoria
author_role author
author2 Gouveia Dal Pino, E. M.
del Valle, Maria Victoria
author2_role author
author
dc.subject.none.fl_str_mv Microquasars
Cosmic ray acceleration
Non thermal mechanisms
Radiation mechanisms
topic Microquasars
Cosmic ray acceleration
Non thermal mechanisms
Radiation mechanisms
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Recent studies have indicated that cosmic ray acceleration by a first-order Fermi process in magnetic reconnection current sheets can be efficient enough in the surrounds of compact sources. In this work, we discuss this acceleration mechanism operating in the core region of galactic black hole binaries (or microquasars) and show the conditions under which this can be more efficient than shock acceleration. In addition, we compare the corresponding acceleration rate with the relevant radiative loss rates obtaining the possible energy cut-off of the accelerated particles and also compute the expected spectral energy distribution (SED) for two sources of this class, namely Cygnus X-1 and Cygnus X-3, considering both leptonic and hadronic processes. The derived SEDs are comparable to the observed ones in the low- and high-energy ranges. Our results suggest that hadronic non-thermal emission due to photomeson production may produce the very high energy gamma-rays in these microquasars.
Fil: Khiali, Behrouz. Universidade Do Sao Paulo. Instituto Astronomia, Geofisica E Ciencias Atmosfericas; Brasil
Fil: Gouveia Dal Pino, E. M.. Universidade Do Sao Paulo. Instituto Astronomia, Geofisica E Ciencias Atmosfericas; Brasil
Fil: del Valle, Maria Victoria. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto Argentino de Radioastronomia (i); Argentina
description Recent studies have indicated that cosmic ray acceleration by a first-order Fermi process in magnetic reconnection current sheets can be efficient enough in the surrounds of compact sources. In this work, we discuss this acceleration mechanism operating in the core region of galactic black hole binaries (or microquasars) and show the conditions under which this can be more efficient than shock acceleration. In addition, we compare the corresponding acceleration rate with the relevant radiative loss rates obtaining the possible energy cut-off of the accelerated particles and also compute the expected spectral energy distribution (SED) for two sources of this class, namely Cygnus X-1 and Cygnus X-3, considering both leptonic and hadronic processes. The derived SEDs are comparable to the observed ones in the low- and high-energy ranges. Our results suggest that hadronic non-thermal emission due to photomeson production may produce the very high energy gamma-rays in these microquasars.
publishDate 2015
dc.date.none.fl_str_mv 2015-02
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/11336/7676
Khiali, Behrouz; Gouveia Dal Pino, E. M.; del Valle, Maria Victoria; A magnetic reconnection model for explaining the multi-wavelength emission of the microquasars Cyg X-1 and Cyg X-3; Oxford University Press; Monthly Notices Of The Royal Astronomical Society; 449; 1; 2-2015; 34-48
0035-8711
url http://hdl.handle.net/11336/7676
identifier_str_mv Khiali, Behrouz; Gouveia Dal Pino, E. M.; del Valle, Maria Victoria; A magnetic reconnection model for explaining the multi-wavelength emission of the microquasars Cyg X-1 and Cyg X-3; Oxford University Press; Monthly Notices Of The Royal Astronomical Society; 449; 1; 2-2015; 34-48
0035-8711
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/http://mnras.oxfordjournals.org/content/449/1/34.abstract
info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stv248
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/zip
application/pdf
dc.publisher.none.fl_str_mv Oxford University Press
publisher.none.fl_str_mv Oxford University Press
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 13.221938

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