1. RODNA
  2. Universidad Nacional de Río Negro
  3. Universidad Nacional de Río Negro
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dc.provenanceUniversidad Nacional de Río Negro-
dc.creatorChristiansen, Hugo-
dc.creatorRomero, Gustavo E.-
dc.creatorOrellana, Mariana D.-
dc.date2007-06-
dc.date.accessioned2020-02-11T14:09:28Z-
dc.date.available2020-02-11T14:09:28Z-
dc.date.issued2007-06-
dc.identifierChristiansen, 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-
dc.identifier1678-4448-
dc.identifierhttp://ref.scielo.org/gsfhzh-
dc.identifierhttp://hdl.handle.net/11336/22323-
dc.identifierhttps://rid.unrn.edu.ar/jspui/handle/20.500.12049/2826-
dc.identifierhttp://dx.doi.org/10.1590/S0103-97332007000400012-
dc.identifier.urihttp://rodna.bn.gov.ar/jspui/handle/bnmm/575886-
dc.descriptionFil: Christiansen, Hugo. Universidade Estadual Do Ceara; Brasil-
dc.descriptionFil: Romero, Gustavo E. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina-
dc.descriptionFil: Romero, Gustavo E. Comisión de Investigaciones Científicas; Argentina-
dc.descriptionFil: Romero, Gustavo E. Instituto Argentino de Radioastronomia; Argentina-
dc.descriptionFil: Orellana, Mariana D. Universidad Nacional de Río Negro; Argentina-
dc.descriptionFil: Orellana, Mariana D. Comisión de Investigaciones Científicas; Argentina-
dc.descriptionFil: Orellana, Mariana D. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina-
dc.descriptionFil: Orellana, Mariana D. Instituto Argentino de Radioastronomía; Argentina-
dc.descriptionA 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.-
dc.formatapplication/pdf-
dc.languageeng-
dc.relation37-
dc.relationBrazilian Journal Of Physics-
dc.rightsinfo:eu-repo/semantics/openAccess-
dc.rightshttps://creativecommons.org/licenses/by-nc-sa/4.0/-
dc.sourcereponame:RID-UNRN (UNRN)-
dc.sourceinstname:Universidad Nacional de Río Negro-
dc.sourceinstacron:UNRN-
dc.source.urihttp://dx.doi.org/10.1590/S0103-97332007000400012-
dc.subjectMicroquasars-
dc.subjectGamma rays-
dc.subjectHadronic Models-
dc.subjectBinary Systems-
dc.subject.::Ciencias Exactas y Naturales::Ciencias Físicas-
dc.titleHigh-energy gamma-ray production in microquasars-
dc.typeinfo:eu-repo/semantics/article-
dc.typeinfo:eu-repo/semantics/acceptedVersion-
dc.typeinfo:ar-repo/semantics/articulo-
dc.about-
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