Photometric variability of the Be star CoRoT-ID 102761769
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Photometric variability of the Be star CoRoT-ID 102761769

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Photometric variability of the Be star CoRoT-ID 102761769

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dc.contributor.author Emilio, M.
dc.contributor.author Andrade, L.
dc.contributor.author Janot-Pacheco, E.
dc.contributor.author Baglin, A.
dc.contributor.author Gutiérrez Soto, Juan
dc.contributor.author Suárez, J. C.
dc.contributor.author De Batz, B.
dc.contributor.author Diago Nebot, Pascual David
dc.contributor.author Fabregat Llueca, Juan
dc.contributor.author Floquet, M.
dc.contributor.author Frémat, Y.
dc.contributor.author Huat, A. L.
dc.contributor.author Hubert, A.M.
dc.contributor.author Espinosa-Lara, F.
dc.contributor.author Leroy, B.
dc.contributor.author Martayan, C.
dc.contributor.author Neiner, C.
dc.contributor.author Semaan, T.
dc.contributor.author Suso, J.
dc.date.accessioned 2015-10-20T13:47:20Z
dc.date.available 2015-10-20T13:47:20Z
dc.date.issued 2010
dc.identifier.uri http://hdl.handle.net/10550/47828
dc.description.abstract Context.Classical Be stars are rapid rotators of spectral type late O to early A and luminosity class V-III, which exhibit Balmer emission lines and often a near infrared excess originating in an equatorially concentrated circumstellar envelope, both produced by sporadic mass ejection episodes. The causes of the abnormal mass loss (the so-called Be phenomenon) are as yet unknown.Aims. For the first time, we can now study in detail Be stars outside the Earth"s atmosphere with sufficient temporal resolution. We investigate the variability of the Be Star CoRoT-ID 102761769 observed with the CoRoT satellite in the exoplanet field during the initial run.Methods.One low-resolution spectrum of the star was obtained with the INT telescope at the Observatorio del Roque de los Muchachos. A time series analysis was performed using both cleanest and singular spectrum analysis algorithms to the CoRoT light curve. To identify the pulsation modes of the observed frequencies, we computed a set of models representative of CoRoT-ID 102761769 by varying its main physical parameters inside the uncertainties discussed.Results.We found two close frequencies related to the star. They are 2.465 c d−1(28.5μHz) and 2.441 c d−1(28.2μHz). The precision to which those frequencies were found is 0.018 c d−1(0.2μHz). The projected stellar rotation was estimated to be 120 km s−1 from the Fourier transform of spectral lines. If CoRoT-ID 102761769 is a typical Galactic Be star it rotates near the critical velocity. The critical rotation frequency of a typical B5-6 star is about 3.5 c d−1(40.5μHz), which implies that the above frequencies are really caused by stellar pulsations rather than star"s rotation.
dc.language.iso eng
dc.relation.ispartof Astronomy and Astrophysics, 2010, vol. 522, p. A43
dc.rights.uri info:eu-repo/semantics/openAccess
dc.source Emilio, M. Andrade, L. Janot-Pacheco, E. Baglin, A. Gutiérrez-Soto, J. Suárez, J. C. De Batz, B. Diago, P. Fabregat, J. Floquet, M. Frémat, Y. Huat, A. L. Hubert, A. M. Espinosa Lara, F. Leroy, B. Martayan, C. Neiner, C. Semaan, T. Suso, J. 2010 Photometric variability of the Be star CoRoT-ID 102761769 Astronomy and Astrophysics 522 A43
dc.subject Partícules (Física nuclear)
dc.subject Esteroides
dc.title Photometric variability of the Be star CoRoT-ID 102761769
dc.type info:eu-repo/semantics/article
dc.date.updated 2015-10-20T13:47:20Z
dc.identifier.idgrec 063077

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