dc.creatordel Palacio, Santiago
dc.creatorBenaglia, Paula
dc.creatorDe Becker, M.
dc.creatorBosch Ramon, Valentí
dc.creatorRomero, Gustavo Esteban
dc.date.accessioned2022-08-08T15:51:02Z
dc.date.accessioned2022-10-15T00:01:42Z
dc.date.available2022-08-08T15:51:02Z
dc.date.available2022-10-15T00:01:42Z
dc.date.created2022-08-08T15:51:02Z
dc.date.issued2022-01
dc.identifierdel Palacio, Santiago; Benaglia, Paula; De Becker, M.; Bosch Ramon, Valentí; Romero, Gustavo Esteban; The non-thermal emission from the colliding-wind binary Apep; Csiro Publishing; Publications Of The Astronomical Society Of Australia; 39; 1-2022; 1-10
dc.identifier1323-3580
dc.identifierhttp://hdl.handle.net/11336/164581
dc.identifierCONICET Digital
dc.identifierCONICET
dc.identifier.urihttps://repositorioslatinoamericanos.uchile.cl/handle/2250/4322402
dc.description.abstractTherecently discovered massive binary system Apep is the most powerful synchrotron emitter among the known Galactic colliding-wind binaries. This makes this particular system of great interest to investigate stellar winds and the non-thermal processes associated with their shocks. This source was detected at various radio bands, and in addition the wind-collision region was resolved by means of very-long baseline interferometric observations. We use a non-thermal emission model for colliding-wind binaries to derive physical properties of this system. The observed morphology in the resolved maps allows us to estimate the system projection angle on the sky to be. The observed radio flux densities also allow us to characterise both the intrinsic synchrotron spectrum of the source and its modifications due to free-free absorption in the stellar winds at low frequencies; from this, we derive mass-loss rates of the stars of and. Finally, the broadband spectral energy distribution is calculated for different combinations of the remaining free parameters, namely the intensity of the magnetic field and the injected power in non-thermal particles. We show that the degeneracy of these two parameters can be solved with observations in the high-energy domain, most likely in the hard X-rays but also possibly in -rays under favourable conditions.
dc.languageeng
dc.publisherCsiro Publishing
dc.relationinfo:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1017/pasa.2021.60
dc.relationinfo:eu-repo/semantics/altIdentifier/ark/https://arxiv.org/pdf/2111.07442.pdf
dc.rightshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.rightsinfo:eu-repo/semantics/openAccess
dc.subjectOUTFLOWS
dc.subjectRADIATION MECHANISMS: NON-THERMAL
dc.subjectRELATIVISTIC PROCESSES
dc.subjectSTARS: MASSIVE
dc.subjectSTARS: WINDS
dc.titleThe non-thermal emission from the colliding-wind binary Apep
dc.typeinfo:eu-repo/semantics/article
dc.typeinfo:ar-repo/semantics/artículo
dc.typeinfo:eu-repo/semantics/publishedVersion


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