Combined stellar structure and atmosphere models for massive stars I. Interior evolution and wind properties on the main sequence

Details Combined stellar structure and atmosphere models for massive stars I. Interior evolution and wind properties on the main sequence Combined stellar structure and atmosphere models for massive stars I. Interior evolution and wind properties on the main sequence

1995-08-29

arxiv.org/abs/astro-ph/9508134v1

Astronomy and Astrophysics

Astrophysics

Submitted to A&A uuencoded, compressed Postscript file including all figures [also available at ftp://obsftp.unige.ch/pub/Prep

Scientific paper

We present the first "combined stellar structure and atmosphere models" (CoStar) for massive stars, which consistently treat the entire mass loosing star from the center out to the asymptotic wind velocity. The models use up-to-date input physics and state-of-the-art techniques to model both the stellar interior and the spherically expanding non--LTE atmosphere including line blanketing. Our models thus yield consistent predictions regarding not only the basic stellar parameters, including abundances, but also theoretical spectra along evolutionary tracks. On the same ground they allow us to study the influence of stellar winds on evolutionary models. In this first paper, we present our method and investigate the wind properties and the interior evolution on the main sequence (MS) at solar metallicity. The wind momentum and energy deposition associated with the MS evolution is given and the adopted wind properties are discussed. From our atmosphere calculations, we also derive theoretical estimates of mass loss driven by radiation pressure. These values are compared with the predictions from recent wind models of the Munich group. We find an overall agreement with most of their results. In addition, our models are better in reproducing the strong wind momentum rates observed in supergiants than those of Puls et al. (1995). A comparison between boundary conditions given by the conventional plane parallel and the new spherically expanding atmosphere approach is made. For the MS evolution the evolutionary tracks and the interior evolution are found to be basically unchanged by the new treatment of the outer layers. Given the small spherical extension of the continuum forming layers in the considered

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