Analysis of the spectral energy distribution from a runaway star bow shock

dc.contributorHenney, W. J.
dc.contributorTorres Peimbert, S.
dc.creatorPeri, Cintia Soledad
dc.creatorAraudo, Anabella Teresa
dc.creatorBenaglia, Paula
dc.creatorRomero, Gustavo Esteban
dc.creatorMartí, Josep
dc.date.accessioned2022-01-13T16:59:35Z
dc.date.accessioned2022-10-15T15:35:17Z
dc.date.available2022-01-13T16:59:35Z
dc.date.available2022-10-15T15:35:17Z
dc.date.created2022-01-13T16:59:35Z
dc.date.issued2011
dc.identifierAnalysis of the spectral energy distribution from a runaway star bow shock; XIII Latin American Regional IAU Meeting; Morelia; México; 2010; 156-156
dc.identifier1405-2059
dc.identifierhttp://hdl.handle.net/11336/150025
dc.identifierCONICET Digital
dc.identifierCONICET
dc.identifier.urihttps://repositorioslatinoamericanos.uchile.cl/handle/2250/4403645
dc.description.abstractThe bow shock produced by the high-mass runaway star BD +43° 3654 (Comerón & Pasquali 2007) has been detected as a non-thermal radio source (S_ν ∝ ν^{-α}, <α>=0.5) and it is the first one of that type ever observed (Benaglia et al. 2010). The non-thermal detection provides evidence of the presence of a magnetic field and relativistic electrons. This population of relativistic particles can produce high-energy (HE) emission.
dc.languageeng
dc.publisherUniversidad Nacional Autónoma de México
dc.relationinfo:eu-repo/semantics/altIdentifier/url/http://www.astroscu.unam.mx/rmaa/RMxAC..40/PDF/RMxAC..40_cperi.pdf
dc.relationinfo:eu-repo/semantics/altIdentifier/url/https://www.astroscu.unam.mx/RMxAC/vol40.html
dc.rightshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.rightsinfo:eu-repo/semantics/openAccess
dc.sourceRevista Mexicana de Astronomía y Astrofísica
dc.subjectMASSIVE STARS
dc.subjectSTELLAR BOW-SHOCKS
dc.titleAnalysis of the spectral energy distribution from a runaway star bow shock
dc.typeinfo:eu-repo/semantics/publishedVersion
dc.typeinfo:eu-repo/semantics/conferenceObject
dc.typeinfo:ar-repo/semantics/documento de conferencia


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