High-energy flares from jet-clump interactions

Autores
Araudo, Anabella Teresa; Bosch Ramon, Valentí; Romero, Gustavo Esteban
Año de publicación
2010
Idioma
inglés
Tipo de recurso
documento de conferencia
Estado
versión publicada
Descripción
High-mass microquasars are binary systems composed by a massive star and a compact object from which relativistic jets are launched. Regarding the companion star, observational evidence supports the idea that winds of hot stars are formed by clumps. Then, these inhomogeneities may interact with the jets producing a flaring activity. In the present contribution we study the interaction between a jet and a clump of the stellar wind in a high-mass microquasar. This interaction produces a shock in the jet, where particles may be accelerated up to relativistic energies. We calculate the spectral energy distributions of the dominant non-thermal processes: synchrotron radiation, inverse Compton scattering, and proton-proton collisions. Significant levels of X- and γ-ray emission are predicted, with luminosities in the different domains up to ˜1034-1035 erg s-1 on a timescale of about ˜1 h. Finally, jet-clump interactions in high-mass microquasars could be detectable at high energies. These phenomena may be behind the fast TeV variability found in some high-mass X-ray binary systems, such as Cygnus X-1, LS 5039 and LS I+61 303. In addition, our model can help to derive information on the properties of jets and clumpy winds.
Fil: Araudo, Anabella Teresa. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: Bosch Ramon, Valentí. Max Planck Institut für Kernphysik,; Alemania
Fil: Romero, Gustavo Esteban. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
High Energy Phenomena in Massive Stars
Jaén
España
Universidad de Jaén
Materia
Microquasars
Binary systems
Relativistic jets
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:11336/231343
Acceder
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network_name_str CONICET Digital (CONICET)
spelling High-energy flares from jet-clump interactionsAraudo, Anabella TeresaBosch Ramon, ValentíRomero, Gustavo EstebanMicroquasarsBinary systemsRelativistic jetshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1High-mass microquasars are binary systems composed by a massive star and a compact object from which relativistic jets are launched. Regarding the companion star, observational evidence supports the idea that winds of hot stars are formed by clumps. Then, these inhomogeneities may interact with the jets producing a flaring activity. In the present contribution we study the interaction between a jet and a clump of the stellar wind in a high-mass microquasar. This interaction produces a shock in the jet, where particles may be accelerated up to relativistic energies. We calculate the spectral energy distributions of the dominant non-thermal processes: synchrotron radiation, inverse Compton scattering, and proton-proton collisions. Significant levels of X- and γ-ray emission are predicted, with luminosities in the different domains up to ˜1034-1035 erg s-1 on a timescale of about ˜1 h. Finally, jet-clump interactions in high-mass microquasars could be detectable at high energies. These phenomena may be behind the fast TeV variability found in some high-mass X-ray binary systems, such as Cygnus X-1, LS 5039 and LS I+61 303. In addition, our model can help to derive information on the properties of jets and clumpy winds.Fil: Araudo, Anabella Teresa. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; ArgentinaFil: Bosch Ramon, Valentí. Max Planck Institut für Kernphysik,; AlemaniaFil: Romero, Gustavo Esteban. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; ArgentinaHigh Energy Phenomena in Massive StarsJaénEspañaUniversidad de JaénAstronomical Society of the PacificMartí, JosepLuque Escamilla, Pedro L.Combi, Jorge Ariel2010info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/conferenceObjectConferenciaBookhttp://purl.org/coar/resource_type/c_5794info:ar-repo/semantics/documentoDeConferenciaapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/231343High-energy flares from jet-clump interactions; High Energy Phenomena in Massive Stars; Jaén; España; 2009; 32-409781583817247CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://ui.adsabs.harvard.edu/abs/2010ASPC..422...32A/abstractinfo:eu-repo/semantics/altIdentifier/url/https://aspbooks.org/custom/publications/paper/422-0032.htmlInternacionalinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-03T09:43:52Zoai:ri.conicet.gov.ar:11336/231343instacron: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:34982025-09-03 09:43:52.53CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv High-energy flares from jet-clump interactions
title High-energy flares from jet-clump interactions
spellingShingle High-energy flares from jet-clump interactions
Araudo, Anabella Teresa
Microquasars
Binary systems
Relativistic jets
title_short High-energy flares from jet-clump interactions
title_full High-energy flares from jet-clump interactions
title_fullStr High-energy flares from jet-clump interactions
title_full_unstemmed High-energy flares from jet-clump interactions
title_sort High-energy flares from jet-clump interactions
dc.creator.none.fl_str_mv Araudo, Anabella Teresa
Bosch Ramon, Valentí
Romero, Gustavo Esteban
author Araudo, Anabella Teresa
author_facet Araudo, Anabella Teresa
Bosch Ramon, Valentí
Romero, Gustavo Esteban
author_role author
author2 Bosch Ramon, Valentí
Romero, Gustavo Esteban
author2_role author
author
dc.contributor.none.fl_str_mv Martí, Josep
Luque Escamilla, Pedro L.
Combi, Jorge Ariel
dc.subject.none.fl_str_mv Microquasars
Binary systems
Relativistic jets
topic Microquasars
Binary systems
Relativistic jets
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv High-mass microquasars are binary systems composed by a massive star and a compact object from which relativistic jets are launched. Regarding the companion star, observational evidence supports the idea that winds of hot stars are formed by clumps. Then, these inhomogeneities may interact with the jets producing a flaring activity. In the present contribution we study the interaction between a jet and a clump of the stellar wind in a high-mass microquasar. This interaction produces a shock in the jet, where particles may be accelerated up to relativistic energies. We calculate the spectral energy distributions of the dominant non-thermal processes: synchrotron radiation, inverse Compton scattering, and proton-proton collisions. Significant levels of X- and γ-ray emission are predicted, with luminosities in the different domains up to ˜1034-1035 erg s-1 on a timescale of about ˜1 h. Finally, jet-clump interactions in high-mass microquasars could be detectable at high energies. These phenomena may be behind the fast TeV variability found in some high-mass X-ray binary systems, such as Cygnus X-1, LS 5039 and LS I+61 303. In addition, our model can help to derive information on the properties of jets and clumpy winds.
Fil: Araudo, Anabella Teresa. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: Bosch Ramon, Valentí. Max Planck Institut für Kernphysik,; Alemania
Fil: Romero, Gustavo Esteban. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
High Energy Phenomena in Massive Stars
Jaén
España
Universidad de Jaén
description High-mass microquasars are binary systems composed by a massive star and a compact object from which relativistic jets are launched. Regarding the companion star, observational evidence supports the idea that winds of hot stars are formed by clumps. Then, these inhomogeneities may interact with the jets producing a flaring activity. In the present contribution we study the interaction between a jet and a clump of the stellar wind in a high-mass microquasar. This interaction produces a shock in the jet, where particles may be accelerated up to relativistic energies. We calculate the spectral energy distributions of the dominant non-thermal processes: synchrotron radiation, inverse Compton scattering, and proton-proton collisions. Significant levels of X- and γ-ray emission are predicted, with luminosities in the different domains up to ˜1034-1035 erg s-1 on a timescale of about ˜1 h. Finally, jet-clump interactions in high-mass microquasars could be detectable at high energies. These phenomena may be behind the fast TeV variability found in some high-mass X-ray binary systems, such as Cygnus X-1, LS 5039 and LS I+61 303. In addition, our model can help to derive information on the properties of jets and clumpy winds.
publishDate 2010
dc.date.none.fl_str_mv 2010
dc.type.none.fl_str_mv info:eu-repo/semantics/publishedVersion
info:eu-repo/semantics/conferenceObject
Conferencia
Book
http://purl.org/coar/resource_type/c_5794
info:ar-repo/semantics/documentoDeConferencia
status_str publishedVersion
format conferenceObject
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/231343
High-energy flares from jet-clump interactions; High Energy Phenomena in Massive Stars; Jaén; España; 2009; 32-40
9781583817247
CONICET Digital
CONICET
url http://hdl.handle.net/11336/231343
identifier_str_mv High-energy flares from jet-clump interactions; High Energy Phenomena in Massive Stars; Jaén; España; 2009; 32-40
9781583817247
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://ui.adsabs.harvard.edu/abs/2010ASPC..422...32A/abstract
info:eu-repo/semantics/altIdentifier/url/https://aspbooks.org/custom/publications/paper/422-0032.html
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
dc.coverage.none.fl_str_mv Internacional
dc.publisher.none.fl_str_mv Astronomical Society of the Pacific
publisher.none.fl_str_mv Astronomical Society of the Pacific
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 13.13397

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