Testing the forward approach in modelling beta Cephei pulsators: setting the stage

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dc.creatorMiglio, A.
dc.creatorMontalban, J.
dc.creatorThoul, A.
dc.date2009-01-14
dc.date.accessioned2026-07-07T12:32:01Z
dc.date.available2026-07-07T12:32:01Z
dc.descriptionThe information on stellar parameters and on the stellar interior we can get by studying pulsating stars depends crucially on the available observational constraints: both seismic constraints precision and number of detected modes, identification, nature of the modes) and "classical" observations (photospheric abundances, effective temperature, luminosity, surface gravity). We consider the case of beta Cephei pulsators and, with the aim of estimating quantitatively how the available observational constraints determine the type and precision of our inferences, we set the stage for Hare&Hound exercises. In this contribution we present preliminary results for one simple case, where we assume as "observed" frequencies a subset of frequencies of a model and then evaluate a seismic merit function on a dense and extensive grid of models of B-type stars. We also compare the behaviour of chi^2 surfaces obtained with and without mode identification.
dc.description3 pages, 1 figure, Comm. in Asteroseismology, Contribution to the Proceedings of the 38th LIAC, HELAS-ESTA, BAG, 2008
dc.identifierhttps://arxiv.org/abs/0901.2072
dc.identifierhttp://arxiv.org/abs/0901.2072
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/216643
dc.subjectSolar and Stellar Astrophysics
dc.titleTesting the forward approach in modelling beta Cephei pulsators: setting the stage
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