Analysis of Balmer Profiles of early type stars

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dc.creatorMolla, Mercedes
dc.creatorDiaz, Angeles I.
dc.creatorAlvarez, Mar Alvarez
dc.creatorDelgado, Rosa Gonzalez
dc.date2000-03-01
dc.date.accessioned2026-07-07T01:52:34Z
dc.date.available2026-07-07T01:52:34Z
dc.descriptionThe spectral energy distribution (SED) of recent star formation regions is dominated by the more massive and early stars (O and B types). These stars show large and very significant absorption features, the most prominent being the recombination lines of H, HeI and HeII. In particular, the shape of their profiles are very dependent on the luminosity of the star. We have explored the potential use of high resolution profiles to discriminate between different luminosity classes and spectral types, by using profiles of the He and Balmer lines. We have calculated growth curves for each of the lines and their dependence on gravity and effective temperature. We show some of these theoretical growth curves and our preliminary conclusions are analyzed and discussed.
dc.description1 pag, Contribution to the conference "Cosmic Evolution and Galaxy Formation: Structure, Interactions and Feedback", Nov. 1999 (Puebla, Mexico), to be published in ASP. Conf. Series, Eds. J. Franco, E. Terlevich. O. Lopez-Cruz, I. Aretxaga
dc.identifierhttps://arxiv.org/abs/astro-ph/0003007
dc.identifierhttp://arxiv.org/abs/astro-ph/0003007
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/662
dc.subjectAstrophysics
dc.titleAnalysis of Balmer Profiles of early type stars
dc.typetext

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