Modeling TeV gamma-rays from LS 5039: An active OB star at the extreme

Autores
Owocki, S. P.; Okazaki, A. T.; Romero, Gustavo Esteban
Año de publicación
2011
Idioma
inglés
Tipo de recurso
documento de conferencia
Estado
versión publicada
Descripción
Perhpas the most extreme examples of "Active OB stars" are the subset of high-mass X-ray binaries - consisting of an OB star plus compact companion - that have recently been observed by Fermi and ground-based Cerenkov telescopes like HESS to be sources of very high energy (VHE; up to 30 TeV!) ã-rays. This paper focuses on the prominent ã-ray source, LS5039, which consists of a massive O6.5V star in a 3.9-day-period, mildly elliptical (e ~ 0.24) orbit with its companion, assumed here to be a black-hole or unmagnetized neutron star. Using 3-D SPH 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 ã-rays is assumed to track this accretion rate, reproduces quite well Fermi observations of the phase variation of ã-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 ã-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 thus making it a strong alternative to the pulsar-wind-shock models commonly invoked to explain such VHE ã-ray emission in massive-star binaries.
Fil: Owocki, S. P.. University of Delaware; Estados Unidos
Fil: Okazaki, A. T.. Hokkai-Gakuen University; Japón
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
IAU Symposium 272: Active OB stars: structure, evolution, mass loss, and critical limits
París
Francia
International Astronomical Union
Materia
OB stars
Gamma-rays
LS 5039 (estrella)
X-ray binaries
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:11336/226581
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/226581
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Modeling TeV gamma-rays from LS 5039: An active OB star at the extremeOwocki, S. P.Okazaki, A. T.Romero, Gustavo EstebanOB starsGamma-raysLS 5039 (estrella)X-ray binarieshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Perhpas the most extreme examples of "Active OB stars" are the subset of high-mass X-ray binaries - consisting of an OB star plus compact companion - that have recently been observed by Fermi and ground-based Cerenkov telescopes like HESS to be sources of very high energy (VHE; up to 30 TeV!) ã-rays. This paper focuses on the prominent ã-ray source, LS5039, which consists of a massive O6.5V star in a 3.9-day-period, mildly elliptical (e ~ 0.24) orbit with its companion, assumed here to be a black-hole or unmagnetized neutron star. Using 3-D SPH 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 ã-rays is assumed to track this accretion rate, reproduces quite well Fermi observations of the phase variation of ã-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 ã-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 thus making it a strong alternative to the pulsar-wind-shock models commonly invoked to explain such VHE ã-ray emission in massive-star binaries.Fil: Owocki, S. P.. University of Delaware; Estados UnidosFil: Okazaki, A. T.. Hokkai-Gakuen University; JapónFil: 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; ArgentinaIAU Symposium 272: Active OB stars: structure, evolution, mass loss, and critical limitsParísFranciaInternational Astronomical UnionCambridge University PressNeiner, C.Wade, G.Meynet, G.Peters, G.2011info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/conferenceObjectSimposioBookhttp://purl.org/coar/resource_type/c_5794info:ar-repo/semantics/documentoDeConferenciaapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/226581Modeling TeV gamma-rays from LS 5039: An active OB star at the extreme; IAU Symposium 272: Active OB stars: structure, evolution, mass loss, and critical limits; París; Francia; 2010; 587-5929780-521-19840-0CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://ui.adsabs.harvard.edu/abs/2011IAUS..272..587O/abstractinfo:eu-repo/semantics/altIdentifier/doi/10.1017/S1743921311011471info:eu-repo/semantics/altIdentifier/url/http://iaus272.obspm.frInternacionalinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:12:52Zoai:ri.conicet.gov.ar:11336/226581instacron: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 10:12:53.163CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Modeling TeV gamma-rays from LS 5039: An active OB star at the extreme
title Modeling TeV gamma-rays from LS 5039: An active OB star at the extreme
spellingShingle Modeling TeV gamma-rays from LS 5039: An active OB star at the extreme
Owocki, S. P.
OB stars
Gamma-rays
LS 5039 (estrella)
X-ray binaries
title_short Modeling TeV gamma-rays from LS 5039: An active OB star at the extreme
title_full Modeling TeV gamma-rays from LS 5039: An active OB star at the extreme
title_fullStr Modeling TeV gamma-rays from LS 5039: An active OB star at the extreme
title_full_unstemmed Modeling TeV gamma-rays from LS 5039: An active OB star at the extreme
title_sort Modeling TeV gamma-rays from LS 5039: An active OB star at the extreme
dc.creator.none.fl_str_mv Owocki, S. P.
Okazaki, A. T.
Romero, Gustavo Esteban
author Owocki, S. P.
author_facet Owocki, S. P.
Okazaki, A. T.
Romero, Gustavo Esteban
author_role author
author2 Okazaki, A. T.
Romero, Gustavo Esteban
author2_role author
author
dc.contributor.none.fl_str_mv Neiner, C.
Wade, G.
Meynet, G.
Peters, G.
dc.subject.none.fl_str_mv OB stars
Gamma-rays
LS 5039 (estrella)
X-ray binaries
topic OB stars
Gamma-rays
LS 5039 (estrella)
X-ray binaries
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Perhpas the most extreme examples of "Active OB stars" are the subset of high-mass X-ray binaries - consisting of an OB star plus compact companion - that have recently been observed by Fermi and ground-based Cerenkov telescopes like HESS to be sources of very high energy (VHE; up to 30 TeV!) ã-rays. This paper focuses on the prominent ã-ray source, LS5039, which consists of a massive O6.5V star in a 3.9-day-period, mildly elliptical (e ~ 0.24) orbit with its companion, assumed here to be a black-hole or unmagnetized neutron star. Using 3-D SPH 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 ã-rays is assumed to track this accretion rate, reproduces quite well Fermi observations of the phase variation of ã-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 ã-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 thus making it a strong alternative to the pulsar-wind-shock models commonly invoked to explain such VHE ã-ray emission in massive-star binaries.
Fil: Owocki, S. P.. University of Delaware; Estados Unidos
Fil: Okazaki, A. T.. Hokkai-Gakuen University; Japón
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
IAU Symposium 272: Active OB stars: structure, evolution, mass loss, and critical limits
París
Francia
International Astronomical Union
description Perhpas the most extreme examples of "Active OB stars" are the subset of high-mass X-ray binaries - consisting of an OB star plus compact companion - that have recently been observed by Fermi and ground-based Cerenkov telescopes like HESS to be sources of very high energy (VHE; up to 30 TeV!) ã-rays. This paper focuses on the prominent ã-ray source, LS5039, which consists of a massive O6.5V star in a 3.9-day-period, mildly elliptical (e ~ 0.24) orbit with its companion, assumed here to be a black-hole or unmagnetized neutron star. Using 3-D SPH 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 ã-rays is assumed to track this accretion rate, reproduces quite well Fermi observations of the phase variation of ã-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 ã-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 thus making it a strong alternative to the pulsar-wind-shock models commonly invoked to explain such VHE ã-ray emission in massive-star binaries.
publishDate 2011
dc.date.none.fl_str_mv 2011
dc.type.none.fl_str_mv info:eu-repo/semantics/publishedVersion
info:eu-repo/semantics/conferenceObject
Simposio
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/11336/226581
Modeling TeV gamma-rays from LS 5039: An active OB star at the extreme; IAU Symposium 272: Active OB stars: structure, evolution, mass loss, and critical limits; París; Francia; 2010; 587-592
9780-521-19840-0
CONICET Digital
CONICET
url http://hdl.handle.net/11336/226581
identifier_str_mv Modeling TeV gamma-rays from LS 5039: An active OB star at the extreme; IAU Symposium 272: Active OB stars: structure, evolution, mass loss, and critical limits; París; Francia; 2010; 587-592
9780-521-19840-0
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/2011IAUS..272..587O/abstract
info:eu-repo/semantics/altIdentifier/doi/10.1017/S1743921311011471
info:eu-repo/semantics/altIdentifier/url/http://iaus272.obspm.fr
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 Cambridge University Press
publisher.none.fl_str_mv Cambridge 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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