Modeling gamma-ray emission from the high-mass X-ray binary LS 5039

Autores
Owocki, Stan; Okazaki, Atsuo; Romero, Gustavo Esteban
Año de publicación
2012
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
A few high-mass X-ray binaries-consisting of an OB star plus compact companion-have been observed by Fermi and ground-based Cerenkov telescopes like High Energy Stereoscopic System (HESS) to be sources of very high energy (VHE; up to 30 TeV) -rays. This paper focuses on the prominent -ray source, LS 5039, which consists of a massive O6.5V star in a 3.9-day-period, mildly elliptical () orbit with its companion, assumed here to be an unmagnetized compact object (e.g., black hole). Using three dimensional smoothed particle hydrodynamics simulations of the Bondi-Hoyle accretion of the O-star wind onto the companion, we find that the orbital phase variation of the accretion follows very closely the simple Bondi-Hoyle-Lyttleton (BHL) rate for the local radius and wind speed. Moreover, a simple model, wherein intrinsic emission of -rays is assumed to track this accretion rate, reproduces quite well Fermi observations of the phase variation of -rays in the energy range 0.1-10 GeV. However for the VHE (0.1-30 TeV) radiation observed by the HESS Cerenkov telescope, it is important to account also for photon-photon interactions between the -rays and the stellar optical/UV radiation, which effectively attenuates much of the strong emission near periastron. When this is included, we find that this simple BHL accretion model also quite naturally fits the HESS light curve, thus making it a strong alternative to the pulsar-wind-shock models commonly invoked to explain such VHE -ray emission in massive-star binaries.
Fil: Owocki, Stan. University of Delaware; Estados Unidos
Fil: Okazaki, Atsuo. Hokkai-Gakuen University; Japón
Fil: Romero, Gustavo Esteban. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Provincia de Buenos Aires. Gobernación. Comision de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomia; Argentina
Materia
Not available
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:11336/17191
Acceder
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network_name_str CONICET Digital (CONICET)
spelling Modeling gamma-ray emission from the high-mass X-ray binary LS 5039Owocki, StanOkazaki, AtsuoRomero, Gustavo EstebanNot availablehttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1A few high-mass X-ray binaries-consisting of an OB star plus compact companion-have been observed by Fermi and ground-based Cerenkov telescopes like High Energy Stereoscopic System (HESS) to be sources of very high energy (VHE; up to 30 TeV) -rays. This paper focuses on the prominent -ray source, LS 5039, which consists of a massive O6.5V star in a 3.9-day-period, mildly elliptical () orbit with its companion, assumed here to be an unmagnetized compact object (e.g., black hole). Using three dimensional smoothed particle hydrodynamics simulations of the Bondi-Hoyle accretion of the O-star wind onto the companion, we find that the orbital phase variation of the accretion follows very closely the simple Bondi-Hoyle-Lyttleton (BHL) rate for the local radius and wind speed. Moreover, a simple model, wherein intrinsic emission of -rays is assumed to track this accretion rate, reproduces quite well Fermi observations of the phase variation of -rays in the energy range 0.1-10 GeV. However for the VHE (0.1-30 TeV) radiation observed by the HESS Cerenkov telescope, it is important to account also for photon-photon interactions between the -rays and the stellar optical/UV radiation, which effectively attenuates much of the strong emission near periastron. When this is included, we find that this simple BHL accretion model also quite naturally fits the HESS light curve, thus making it a strong alternative to the pulsar-wind-shock models commonly invoked to explain such VHE -ray emission in massive-star binaries.Fil: Owocki, Stan. University of Delaware; Estados UnidosFil: Okazaki, Atsuo. Hokkai-Gakuen University; JapónFil: Romero, Gustavo Esteban. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Provincia de Buenos Aires. Gobernación. Comision de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomia; ArgentinaThe korean Space Science Society2012-03info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/17191Owocki, Stan; Okazaki, Atsuo; Romero, Gustavo Esteban; Modeling gamma-ray emission from the high-mass X-ray binary LS 5039; The korean Space Science Society; Journal of Astronomy and Space Sciences; 29; 1; 3-2012; 51-552093-5587enginfo:eu-repo/semantics/altIdentifier/doi/10.5140/JASS.2012.29.1.051info:eu-repo/semantics/altIdentifier/url/http://koreascience.or.kr/article/ArticleFullRecord.jsp?cn=OJOOBS_2012_v29n1_51info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:10:37Zoai:ri.conicet.gov.ar:11336/17191instacron: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 10:10:37.704CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Modeling gamma-ray emission from the high-mass X-ray binary LS 5039
title Modeling gamma-ray emission from the high-mass X-ray binary LS 5039
spellingShingle Modeling gamma-ray emission from the high-mass X-ray binary LS 5039
Owocki, Stan
Not available
title_short Modeling gamma-ray emission from the high-mass X-ray binary LS 5039
title_full Modeling gamma-ray emission from the high-mass X-ray binary LS 5039
title_fullStr Modeling gamma-ray emission from the high-mass X-ray binary LS 5039
title_full_unstemmed Modeling gamma-ray emission from the high-mass X-ray binary LS 5039
title_sort Modeling gamma-ray emission from the high-mass X-ray binary LS 5039
dc.creator.none.fl_str_mv Owocki, Stan
Okazaki, Atsuo
Romero, Gustavo Esteban
author Owocki, Stan
author_facet Owocki, Stan
Okazaki, Atsuo
Romero, Gustavo Esteban
author_role author
author2 Okazaki, Atsuo
Romero, Gustavo Esteban
author2_role author
author
dc.subject.none.fl_str_mv Not available
topic Not available
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv A few high-mass X-ray binaries-consisting of an OB star plus compact companion-have been observed by Fermi and ground-based Cerenkov telescopes like High Energy Stereoscopic System (HESS) to be sources of very high energy (VHE; up to 30 TeV) -rays. This paper focuses on the prominent -ray source, LS 5039, which consists of a massive O6.5V star in a 3.9-day-period, mildly elliptical () orbit with its companion, assumed here to be an unmagnetized compact object (e.g., black hole). Using three dimensional smoothed particle hydrodynamics simulations of the Bondi-Hoyle accretion of the O-star wind onto the companion, we find that the orbital phase variation of the accretion follows very closely the simple Bondi-Hoyle-Lyttleton (BHL) rate for the local radius and wind speed. Moreover, a simple model, wherein intrinsic emission of -rays is assumed to track this accretion rate, reproduces quite well Fermi observations of the phase variation of -rays in the energy range 0.1-10 GeV. However for the VHE (0.1-30 TeV) radiation observed by the HESS Cerenkov telescope, it is important to account also for photon-photon interactions between the -rays and the stellar optical/UV radiation, which effectively attenuates much of the strong emission near periastron. When this is included, we find that this simple BHL accretion model also quite naturally fits the HESS light curve, thus making it a strong alternative to the pulsar-wind-shock models commonly invoked to explain such VHE -ray emission in massive-star binaries.
Fil: Owocki, Stan. University of Delaware; Estados Unidos
Fil: Okazaki, Atsuo. Hokkai-Gakuen University; Japón
Fil: Romero, Gustavo Esteban. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Provincia de Buenos Aires. Gobernación. Comision de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomia; Argentina
description A few high-mass X-ray binaries-consisting of an OB star plus compact companion-have been observed by Fermi and ground-based Cerenkov telescopes like High Energy Stereoscopic System (HESS) to be sources of very high energy (VHE; up to 30 TeV) -rays. This paper focuses on the prominent -ray source, LS 5039, which consists of a massive O6.5V star in a 3.9-day-period, mildly elliptical () orbit with its companion, assumed here to be an unmagnetized compact object (e.g., black hole). Using three dimensional smoothed particle hydrodynamics simulations of the Bondi-Hoyle accretion of the O-star wind onto the companion, we find that the orbital phase variation of the accretion follows very closely the simple Bondi-Hoyle-Lyttleton (BHL) rate for the local radius and wind speed. Moreover, a simple model, wherein intrinsic emission of -rays is assumed to track this accretion rate, reproduces quite well Fermi observations of the phase variation of -rays in the energy range 0.1-10 GeV. However for the VHE (0.1-30 TeV) radiation observed by the HESS Cerenkov telescope, it is important to account also for photon-photon interactions between the -rays and the stellar optical/UV radiation, which effectively attenuates much of the strong emission near periastron. When this is included, we find that this simple BHL accretion model also quite naturally fits the HESS light curve, thus making it a strong alternative to the pulsar-wind-shock models commonly invoked to explain such VHE -ray emission in massive-star binaries.
publishDate 2012
dc.date.none.fl_str_mv 2012-03
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/11336/17191
Owocki, Stan; Okazaki, Atsuo; Romero, Gustavo Esteban; Modeling gamma-ray emission from the high-mass X-ray binary LS 5039; The korean Space Science Society; Journal of Astronomy and Space Sciences; 29; 1; 3-2012; 51-55
2093-5587
url http://hdl.handle.net/11336/17191
identifier_str_mv Owocki, Stan; Okazaki, Atsuo; Romero, Gustavo Esteban; Modeling gamma-ray emission from the high-mass X-ray binary LS 5039; The korean Space Science Society; Journal of Astronomy and Space Sciences; 29; 1; 3-2012; 51-55
2093-5587
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.5140/JASS.2012.29.1.051
info:eu-repo/semantics/altIdentifier/url/http://koreascience.or.kr/article/ArticleFullRecord.jsp?cn=OJOOBS_2012_v29n1_51
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.publisher.none.fl_str_mv The korean Space Science Society
publisher.none.fl_str_mv The korean Space Science Society
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 13.260194

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