Please use this identifier to cite or link to this item: http://hdl.handle.net/2445/122845
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dc.contributor.authorZabalza de Torres, Víctor-
dc.contributor.authorBosch i Ramon, Valentí-
dc.contributor.authorParedes i Poy, Josep Maria-
dc.date.accessioned2018-06-07T14:59:15Z-
dc.date.available2018-06-07T14:59:15Z-
dc.date.issued2011-12-10-
dc.identifier.issn0004-637X-
dc.identifier.urihttp://hdl.handle.net/2445/122845-
dc.description.abstractGamma-ray loud X-ray binaries are binary systems that show non-thermal broadband emission from radio to gamma rays. If the system comprises a massive star and a young non-accreting pulsar, their winds will collide producing broadband non-thermal emission, most likely originated in the shocked pulsar wind. Thermal X-ray emission is expected from the shocked stellar wind, but until now it has neither been detected nor studied in the context of gamma-ray binaries. We present a semi-analytic model of the thermal X-ray emission from the shocked stellar wind in pulsar gamma-ray binaries, and find that the thermal X-ray emission increases monotonically with the pulsar spin-down luminosity, reaching luminosities of the order of 10^33 erg/s. The lack of thermal features in the X-ray spectrum of gamma-ray binaries can then be used to constrain the properties of the pulsar and stellar winds. By fitting the observed X-ray spectra of gamma-ray binaries with a source model composed of an absorbed non-thermal power law and the computed thermal X-ray emission, we are able to derive upper limits on the spin-down luminosity of the putative pulsar. We applied this method to LS 5039, the only gamma-ray binary with a radial, powerful wind, and obtain an upper limit on the pulsar spin-down luminosity of ~6x10^36 erg/s. Given the energetic constraints from its high-energy gamma-ray emission, a non-thermal to spin-down luminosity ratio very close to unity may be required.-
dc.format.extent9 p.-
dc.format.mimetypeapplication/pdf-
dc.language.isoeng-
dc.publisherInstitute of Physics (IOP)-
dc.relation.isformatofReproducció del document publicat a: https://doi.org/10.1088/0004-637X/743/1/7-
dc.relation.ispartofAstrophysical Journal, 2011, vol. 743, num. 7-
dc.relation.urihttps://doi.org/10.1088/0004-637X/743/1/7-
dc.rights(c) American Astronomical Society, 2011-
dc.subject.classificationEstels binaris de raigs X-
dc.subject.classificationRaigs gamma-
dc.subject.otherX-ray binaries-
dc.subject.otherGamma rays-
dc.titleThermal X-Ray emission from the shocked stellar wind of pulsar gamma-ray binaries-
dc.typeinfo:eu-repo/semantics/article-
dc.typeinfo:eu-repo/semantics/publishedVersion-
dc.identifier.idgrec602763-
dc.date.updated2018-06-07T14:59:15Z-
dc.rights.accessRightsinfo:eu-repo/semantics/openAccess-
Appears in Collections:Articles publicats en revistes (Física Quàntica i Astrofísica)

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