High-energy gamma-ray production in microquasars
- Autores
- Christiansen, Hugo; Romero, Gustavo E.; Orellana, Mariana Dominga
- Año de publicación
- 2007
- Idioma
- español castellano
- Tipo de recurso
- artículo
- Estado
- versión aceptada
- Descripción
- Fil: Christiansen, Hugo. Universidade Estadual Do Ceara; Brasil
Fil: Romero, Gustavo E. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina
Fil: Romero, Gustavo E. Comisión de Investigaciones Científicas; Argentina
Fil: Romero, Gustavo E. Instituto Argentino de Radioastronomia; Argentina
Fil: Orellana, Mariana D. Universidad Nacional de Río Negro; Argentina
Fil: Orellana, Mariana D. Comisión de Investigaciones Científicas; Argentina
Fil: Orellana, Mariana D. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina
Fil: Orellana, Mariana D. Instituto Argentino de Radioastronomía; Argentina
A hadronic model for gamma-ray production in microquasars is presented. Microquasars are galactic binary systems with jets, which have, presumably, hadronic components. We consider a microquasar formed by a neutron star that accretes matter from the equatorial wind of a Be primary star. The collision between the jet, emitted by the compact object, and the dense equatorial disk of the companion massive star is responsible for the gamma-ray production. Gamma-rays result from the decay of neutral pions produced in relativistic pp interactions arising from this collision all along the orbit. Assuming a simple, positional independent set of parameters, our calculations are consistent with a peak of gamma-ray flux at the periastron passage with a secondary maximum near apastron. Under this assumption, gamma-ray signals would be in contrast with the radio/X-ray outbursts which peak clearly after periastron. We finally calculate the opacity of the ambient photon field to the propagation of the gamma-rays. The spectral energy distribution appears strongly attenuated in a wide band (50 GeV - 50 TeV) due to local absorption. These spectral features should be detectable by an instrument like MAGIC through exposures integrated along several periastron passages. - Materia
-
Ciencias Físicas
Microquasars
Gamma rays
Hadronic Models
Binary Systems
Ciencias Físicas - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/4.0/
- Repositorio
.jpg)
- Institución
- Universidad Nacional de Río Negro
- OAI Identificador
- oai:rid.unrn.edu.ar:20.500.12049/2826
Ver los metadatos del registro completo
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High-energy gamma-ray production in microquasarsChristiansen, HugoRomero, Gustavo E.Orellana, Mariana DomingaCiencias FísicasMicroquasarsGamma raysHadronic ModelsBinary SystemsCiencias FísicasFil: Christiansen, Hugo. Universidade Estadual Do Ceara; BrasilFil: Romero, Gustavo E. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; ArgentinaFil: Romero, Gustavo E. Comisión de Investigaciones Científicas; ArgentinaFil: Romero, Gustavo E. Instituto Argentino de Radioastronomia; ArgentinaFil: Orellana, Mariana D. Universidad Nacional de Río Negro; ArgentinaFil: Orellana, Mariana D. Comisión de Investigaciones Científicas; ArgentinaFil: Orellana, Mariana D. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; ArgentinaFil: Orellana, Mariana D. Instituto Argentino de Radioastronomía; ArgentinaA hadronic model for gamma-ray production in microquasars is presented. Microquasars are galactic binary systems with jets, which have, presumably, hadronic components. We consider a microquasar formed by a neutron star that accretes matter from the equatorial wind of a Be primary star. The collision between the jet, emitted by the compact object, and the dense equatorial disk of the companion massive star is responsible for the gamma-ray production. Gamma-rays result from the decay of neutral pions produced in relativistic pp interactions arising from this collision all along the orbit. Assuming a simple, positional independent set of parameters, our calculations are consistent with a peak of gamma-ray flux at the periastron passage with a secondary maximum near apastron. Under this assumption, gamma-ray signals would be in contrast with the radio/X-ray outbursts which peak clearly after periastron. We finally calculate the opacity of the ambient photon field to the propagation of the gamma-rays. The spectral energy distribution appears strongly attenuated in a wide band (50 GeV - 50 TeV) due to local absorption. These spectral features should be detectable by an instrument like MAGIC through exposures integrated along several periastron passages.2007-06info:eu-repo/semantics/articleinfo:eu-repo/semantics/acceptedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfChristiansen, Hugo., Romero, Gustavo E. & Orellana, Mariana D. (2007). High-energy gamma-ray production in microquasars. Sociedad Brasileira Fisica. Brazilian Journal Of Physics; 37; 2B; 545-5481678-4448http://ref.scielo.org/gsfhzhhttp://hdl.handle.net/11336/22323https://rid.unrn.edu.ar/jspui/handle/20.500.12049/2826http://dx.doi.org/10.1590/S0103-97332007000400012spa37Brazilian Journal Of Physicsinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/4.0/reponame:RID-UNRN (UNRN)instname:Universidad Nacional de Río Negro2025-09-29T14:29:05Zoai:rid.unrn.edu.ar:20.500.12049/2826instacron:UNRNInstitucionalhttps://rid.unrn.edu.ar/jspui/Universidad públicaNo correspondehttps://rid.unrn.edu.ar/oai/snrdrid@unrn.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:43692025-09-29 14:29:05.337RID-UNRN (UNRN) - Universidad Nacional de Río Negrofalse |
| dc.title.none.fl_str_mv |
High-energy gamma-ray production in microquasars |
| title |
High-energy gamma-ray production in microquasars |
| spellingShingle |
High-energy gamma-ray production in microquasars Christiansen, Hugo Ciencias Físicas Microquasars Gamma rays Hadronic Models Binary Systems Ciencias Físicas |
| title_short |
High-energy gamma-ray production in microquasars |
| title_full |
High-energy gamma-ray production in microquasars |
| title_fullStr |
High-energy gamma-ray production in microquasars |
| title_full_unstemmed |
High-energy gamma-ray production in microquasars |
| title_sort |
High-energy gamma-ray production in microquasars |
| dc.creator.none.fl_str_mv |
Christiansen, Hugo Romero, Gustavo E. Orellana, Mariana Dominga |
| author |
Christiansen, Hugo |
| author_facet |
Christiansen, Hugo Romero, Gustavo E. Orellana, Mariana Dominga |
| author_role |
author |
| author2 |
Romero, Gustavo E. Orellana, Mariana Dominga |
| author2_role |
author author |
| dc.subject.none.fl_str_mv |
Ciencias Físicas Microquasars Gamma rays Hadronic Models Binary Systems Ciencias Físicas |
| topic |
Ciencias Físicas Microquasars Gamma rays Hadronic Models Binary Systems Ciencias Físicas |
| dc.description.none.fl_txt_mv |
Fil: Christiansen, Hugo. Universidade Estadual Do Ceara; Brasil Fil: Romero, Gustavo E. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina Fil: Romero, Gustavo E. Comisión de Investigaciones Científicas; Argentina Fil: Romero, Gustavo E. Instituto Argentino de Radioastronomia; Argentina Fil: Orellana, Mariana D. Universidad Nacional de Río Negro; Argentina Fil: Orellana, Mariana D. Comisión de Investigaciones Científicas; Argentina Fil: Orellana, Mariana D. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina Fil: Orellana, Mariana D. Instituto Argentino de Radioastronomía; Argentina A hadronic model for gamma-ray production in microquasars is presented. Microquasars are galactic binary systems with jets, which have, presumably, hadronic components. We consider a microquasar formed by a neutron star that accretes matter from the equatorial wind of a Be primary star. The collision between the jet, emitted by the compact object, and the dense equatorial disk of the companion massive star is responsible for the gamma-ray production. Gamma-rays result from the decay of neutral pions produced in relativistic pp interactions arising from this collision all along the orbit. Assuming a simple, positional independent set of parameters, our calculations are consistent with a peak of gamma-ray flux at the periastron passage with a secondary maximum near apastron. Under this assumption, gamma-ray signals would be in contrast with the radio/X-ray outbursts which peak clearly after periastron. We finally calculate the opacity of the ambient photon field to the propagation of the gamma-rays. The spectral energy distribution appears strongly attenuated in a wide band (50 GeV - 50 TeV) due to local absorption. These spectral features should be detectable by an instrument like MAGIC through exposures integrated along several periastron passages. |
| description |
Fil: Christiansen, Hugo. Universidade Estadual Do Ceara; Brasil |
| publishDate |
2007 |
| dc.date.none.fl_str_mv |
2007-06 |
| dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/acceptedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
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article |
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acceptedVersion |
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Christiansen, Hugo., Romero, Gustavo E. & Orellana, Mariana D. (2007). High-energy gamma-ray production in microquasars. Sociedad Brasileira Fisica. Brazilian Journal Of Physics; 37; 2B; 545-548 1678-4448 http://ref.scielo.org/gsfhzh http://hdl.handle.net/11336/22323 https://rid.unrn.edu.ar/jspui/handle/20.500.12049/2826 http://dx.doi.org/10.1590/S0103-97332007000400012 |
| identifier_str_mv |
Christiansen, Hugo., Romero, Gustavo E. & Orellana, Mariana D. (2007). High-energy gamma-ray production in microquasars. Sociedad Brasileira Fisica. Brazilian Journal Of Physics; 37; 2B; 545-548 1678-4448 |
| url |
http://ref.scielo.org/gsfhzh http://hdl.handle.net/11336/22323 https://rid.unrn.edu.ar/jspui/handle/20.500.12049/2826 http://dx.doi.org/10.1590/S0103-97332007000400012 |
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37 Brazilian Journal Of Physics |
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