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dc.date.accessioned 2019-11-07T18:27:58Z
dc.date.available 2019-11-07T18:27:58Z
dc.date.issued 2013
dc.identifier.uri http://sedici.unlp.edu.ar/handle/10915/85187
dc.description.abstract We study the interaction of early-type stars with the jets of active galactic nuclei. A bow-shock will form as a consequence of the interaction of the jet with the winds of stars and particles can be accelerated up to relativistic energies in these shocks. We compute the non-thermal radiation produced by relativistic electrons from radio to gamma-rays. This radiation may be significant, and its detection might yield information on the properties of the stellar population in the galaxy nucleus, as well as on the relativistic jet. This emission is expected to be relevant for nearby non-blazar sources. en
dc.language en es
dc.subject Gamma rays es
dc.subject X-ray es
dc.subject Binary LS es
dc.title Gamma-ray emission from early-type stars interacting with AGN jets en
dc.type Articulo es
sedici.identifier.other doi:10.1051/epjconf/20136105014 es
sedici.identifier.other eid:2-s2.0-84893270033 es
sedici.identifier.issn 2101-6275 es
sedici.creator.person Araudo, Anabella Teresa es
sedici.creator.person Bosch Ramon, Valentí es
sedici.creator.person Romero, Gustavo Esteban es
sedici.subject.materias Ciencias Astronómicas es
sedici.description.fulltext true es
mods.originInfo.place Facultad de Ciencias Astronómicas y Geofísicas es
mods.originInfo.place Instituto Argentino de Radioastronomía es
sedici.subtype Articulo es
sedici.rights.license Creative Commons Attribution 4.0 International (CC BY 4.0)
sedici.rights.uri http://creativecommons.org/licenses/by/4.0/
sedici.relation.event International Symposium on the Innermost Regions of Relativistic Jets and Their Magnetic Fields (Granada, Spain, 10-14 June, 2013) es
sedici.description.peerReview peer-review es
sedici.relation.journalTitle EPJ Web of Conferences es
sedici.relation.journalVolumeAndIssue vol. 61 es


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Creative Commons Attribution 4.0 International (CC BY 4.0) Excepto donde se diga explícitamente, este item se publica bajo la siguiente licencia Creative Commons Attribution 4.0 International (CC BY 4.0)