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dc.contributor.authorOrellana, Mariana Dominga-
dc.contributor.authorBordas, Pol-
dc.contributor.authorBosch Ramon, Valentí-
dc.contributor.authorRomero, Gustavo E.-
dc.contributor.authorParedes, Josep M.-
dc.date.accessioned2019-08-14T17:31:05Z-
dc.date.available2019-08-14T17:31:05Z-
dc.date.issued2007-10-03-
dc.identifier.citationOrellana, Mariana D., Bordas, Pol., Bosch Ramon, Valentí., Romero, Gustavo E. & Paredes, Josep M. (2007). Leptonic secondary emission in a hadronic microquasar model. EDP Sciences; Astronomy and Astrophysics; 476; 1; 9-15es_ES
dc.identifier.issn0004-6361es_ES
dc.identifier.urihttps://www.aanda.org/articles/aa/abs/2007/46/aa8495-07/aa8495-07.html-
dc.identifier.urihttp://hdl.handle.net/11336/29338-
dc.identifier.urihttps://rid.unrn.edu.ar/jspui/handle/20.500.12049/2827-
dc.format.extentp. 9-15es_ES
dc.format.mediumimpresoes_ES
dc.format.mediumdigitales_ES
dc.language.isoenges_ES
dc.titleLeptonic secondary emission in a hadronic microquasar modeles_ES
dc.typeArticuloes_ES
dc.rights.licensehttps://creativecommons.org/licenses/by-nc-sa/4.0/es_ES
dc.description.filiationFil: Orellana, Mariana D. Universidad Nacional de Río Negro; Argentinaes_ES
dc.description.filiationFil: Orellana, Mariana D. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentinaes_ES
dc.description.filiationFil: Orellana, Mariana D. Instituto Argentino de Radioastronomia; Argentinaes_ES
dc.description.filiationFil: Bordas, Pol. Universidad de Barcelona; Españaes_ES
dc.description.filiationFil: Bosch Ramon, Valentí. Max Planck Institut für Kernphysik; Alemaniaes_ES
dc.description.filiationFil: Romero, Gustavo E. Comisión de Investigaciones Científicas; Argentinaes_ES
dc.description.filiationFil: Romero, Gustavo E. Instituto Argentino de Radioastronomia; Argentinaes_ES
dc.description.filiationFil: Romero, Gustavo E. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentinaes_ES
dc.description.filiationFil: Paredes, Josep M. Universidad de Barcelona; Españaes_ES
dc.subject.keywordRadiation Mechanismses_ES
dc.subject.keywordGamma Rayses_ES
dc.subject.keywordBinary Starses_ES
dc.type.versioninfo:eu-repo/semantics/acceptedVersiones_ES
dc.subject.materiaCiencias Físicases_ES
dc.origin.lugarDesarrolloUniversidad Nacional de Río Negroes_ES
dc.relation.journalissue476es_ES
dc.description.reviewtruees_ES
dc.description.resumenContext. It has been proposed that the origin of the very high-energy photons emitted from high-mass X-ray binaries with jet-like features, so-called microquasars (MQs), is related to hadronic interactions between relativistic protons in the jet and cold protons of the stellar wind. Leptonic secondary emission should be calculated in a complete hadronic model that include the effects of pairs from charged pion decays inside the jets and the emission from pairs generated by gamma-ray absorption in the photosphere of the system. Aims. We aim at predicting the broadband spectrum from a general hadronic microquasar model, taking into account the emission from secondaries created by charged pion decay inside the jet. Methods. The particle energy distribution for secondary leptons injected along the jets is consistently derived taking the energy losses into account. We also compute the spectral energy distribution resulting from these leptons is calculated after assuming different values of the magnetic field inside the jets. The spectrum of the gamma-rays produced by neutral pion-decay and processed by electromagnetic cascades under the stellar photon field. Results. We show that the secondary emission can dominate the spectral energy distribution at low energies ( ∼ 1 MeV). At high energies, the production spectrum can be significantly distorted by the effect of electromagnetic cascades. These effects are phase-dependent, and some variability modulated by the orbital period is predicted.es_ES
dc.identifier.doihttp://dx.doi.org/10.1051/0004-6361:20078495-
dc.relation.journalTitleAstronomy and Astrophysicses_ES
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