Lepto-hadronic model for the broadband emission of Cygnus X-1

Context. Cygnus X-1 is a well-observed microquasar. Broadband observations at all wavelengths have been collected over the years.The origin of the MeV tail observed with COMPTEL and INTEGRAL is still under debate and it has mostly been attributed to thecorona, although its high degree of polarizatio...

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Autores: Pepe, Carolina, Vila, Gabriela Soledad, Romero, Gustavo Esteban
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2015
País:Argentina
Institución:Consejo Nacional de Investigaciones Científicas y Técnicas
Repositorio:CONICET Digital (CONICET)
Idioma:inglés
OAI Identifier:oai:ri.conicet.gov.ar:11336/6977
Acceso en línea:http://hdl.handle.net/11336/6977
Access Level:acceso embargado
Palabra clave:Gamma rays
Nonthermal mechanisms
X-ray binaries
Cygnus X-1 (microquasar)
Microquasars
https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
id AR_ec944bee2209287fac1595372aaf002c
oai_identifier_str oai:ri.conicet.gov.ar:11336/6977
network_acronym_str AR
network_name_str Argentina
repository_id_str
spelling Lepto-hadronic model for the broadband emission of Cygnus X-1Pepe, CarolinaVila, Gabriela SoledadRomero, Gustavo EstebanGamma raysNonthermal mechanismsX-ray binariesCygnus X-1 (microquasar)Microquasarshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. Cygnus X-1 is a well-observed microquasar. Broadband observations at all wavelengths have been collected over the years.The origin of the MeV tail observed with COMPTEL and INTEGRAL is still under debate and it has mostly been attributed to thecorona, although its high degree of polarization suggests that it is synchrotron radiation from a jet. The origin of the transient emissionabove ∼100 GeV is also unclear.Aims. We aim to clarify the origin of the broadband spectral energy distribution (SED) of Cygnus X-1, focusing particularly on thegamma-ray emission, and to gain information on the physical conditions inside the jets.Methods. We developed a lepto-hadronic, inhomogeneous jet model and applied it to the non-thermal SED of Cygnus X-1. Wecalculated the contributions to the SED of both protons and electrons accelerated in an extended region of the jet. We also estimatedthe radiation of charged secondaries produced in hadronic interactions through several radiative processes. Absorption effects wereconsidered. We produced synthetic maps of the jets at radio wavelengths.Results. We find two sets of model parameters that lead to good fits of the SED. One of the models fits all the observations, includingthe MeV tail. This model also predicts hadronic gamma-ray emission slightly below the current upper limits. The flux predicted at8.4 GHz is in agreement with the observations available in the literature, although the synthetic source is more compact than theimaged radio jet.Conclusions. Our results show that the MeV emission in Cygnus X-1 may be jet synchrotron radiation. This depends mainly on thestrength of the jet magnetic field and the location of the injection region of the relativistic particles. Our calculations show that theremust be energetic electrons in the jets quite far from the black hole.Fil: Pepe, Carolina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto Argentino de Radioastronomia (i); ArgentinaFil: Vila, Gabriela Soledad. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto Argentino de Radioastronomia (i); ArgentinaFil: Romero, Gustavo Esteban. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto Argentino de Radioastronomia (i); Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaEDP Sciences2015-12info:eu-repo/date/embargoEnd/2016-12-30info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/6977Pepe, Carolina; Vila, Gabriela Soledad; Romero, Gustavo Esteban; Lepto-hadronic model for the broadband emission of Cygnus X-1; EDP Sciences; Astronomy And Astrophysics; 584; 95; 12-2015; 1-110004-6361enginfo:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2015/12/aa27156-15/aa27156-15.htmlinfo:eu-repo/semantics/altIdentifier/doi/info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201527156info:eu-repo/semantics/embargoedAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2024-05-08T13:40:35Zoai:ri.conicet.gov.ar:11336/6977instacron: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:34982024-05-08 13:40:35.867CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Lepto-hadronic model for the broadband emission of Cygnus X-1
title Lepto-hadronic model for the broadband emission of Cygnus X-1
spellingShingle Lepto-hadronic model for the broadband emission of Cygnus X-1
Pepe, Carolina
Gamma rays
Nonthermal mechanisms
X-ray binaries
Cygnus X-1 (microquasar)
Microquasars
https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
title_short Lepto-hadronic model for the broadband emission of Cygnus X-1
title_full Lepto-hadronic model for the broadband emission of Cygnus X-1
title_fullStr Lepto-hadronic model for the broadband emission of Cygnus X-1
title_full_unstemmed Lepto-hadronic model for the broadband emission of Cygnus X-1
title_sort Lepto-hadronic model for the broadband emission of Cygnus X-1
dc.creator.none.fl_str_mv Pepe, Carolina
Vila, Gabriela Soledad
Romero, Gustavo Esteban
author Pepe, Carolina
author_facet Pepe, Carolina
Vila, Gabriela Soledad
Romero, Gustavo Esteban
author_role author
author2 Vila, Gabriela Soledad
Romero, Gustavo Esteban
author2_role author
author
dc.subject.none.fl_str_mv Gamma rays
Nonthermal mechanisms
X-ray binaries
Cygnus X-1 (microquasar)
Microquasars
https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
topic Gamma rays
Nonthermal mechanisms
X-ray binaries
Cygnus X-1 (microquasar)
Microquasars
https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
description Context. Cygnus X-1 is a well-observed microquasar. Broadband observations at all wavelengths have been collected over the years.The origin of the MeV tail observed with COMPTEL and INTEGRAL is still under debate and it has mostly been attributed to thecorona, although its high degree of polarization suggests that it is synchrotron radiation from a jet. The origin of the transient emissionabove ∼100 GeV is also unclear.Aims. We aim to clarify the origin of the broadband spectral energy distribution (SED) of Cygnus X-1, focusing particularly on thegamma-ray emission, and to gain information on the physical conditions inside the jets.Methods. We developed a lepto-hadronic, inhomogeneous jet model and applied it to the non-thermal SED of Cygnus X-1. Wecalculated the contributions to the SED of both protons and electrons accelerated in an extended region of the jet. We also estimatedthe radiation of charged secondaries produced in hadronic interactions through several radiative processes. Absorption effects wereconsidered. We produced synthetic maps of the jets at radio wavelengths.Results. We find two sets of model parameters that lead to good fits of the SED. One of the models fits all the observations, includingthe MeV tail. This model also predicts hadronic gamma-ray emission slightly below the current upper limits. The flux predicted at8.4 GHz is in agreement with the observations available in the literature, although the synthetic source is more compact than theimaged radio jet.Conclusions. Our results show that the MeV emission in Cygnus X-1 may be jet synchrotron radiation. This depends mainly on thestrength of the jet magnetic field and the location of the injection region of the relativistic particles. Our calculations show that theremust be energetic electrons in the jets quite far from the black hole.
publishDate 2015
dc.date.none.fl_str_mv 2015-12
info:eu-repo/date/embargoEnd/2016-12-30
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/11336/6977
Pepe, Carolina; Vila, Gabriela Soledad; Romero, Gustavo Esteban; Lepto-hadronic model for the broadband emission of Cygnus X-1; EDP Sciences; Astronomy And Astrophysics; 584; 95; 12-2015; 1-11
0004-6361
url http://hdl.handle.net/11336/6977
identifier_str_mv Pepe, Carolina; Vila, Gabriela Soledad; Romero, Gustavo Esteban; Lepto-hadronic model for the broadband emission of Cygnus X-1; EDP Sciences; Astronomy And Astrophysics; 584; 95; 12-2015; 1-11
0004-6361
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2015/12/aa27156-15/aa27156-15.html
info:eu-repo/semantics/altIdentifier/doi/
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201527156
dc.rights.none.fl_str_mv info:eu-repo/semantics/embargoedAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv embargoedAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv 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
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
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 15,81155

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