Volume 508, Number 2, December III 2009
|Page(s)||841 - 848|
|Section||Stellar structure and evolution|
|Published online||21 October 2009|
X-ray emission from hydrodynamical simulations in non-LTE wind models
Ústav teoretické fyziky a astrofyziky, Masarykova univerzita, Kotlářská 2, 611 37 Brno, Czech Republic e-mail: firstname.lastname@example.org
2 Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Straße 24/25, 14476 Potsdam-Golm, Germany
3 Astronomický ústav, Akademie věd České republiky, 251 65 Ondřejov, Czech Republic
Accepted: 9 September 2009
Hot stars are sources of X-ray emission originating in their winds. Although hydrodynamical simulations that are able to predict this X-ray emission are available, the inclusion of X-rays in stationary wind models is usually based on simplifying approximations. To improve this, we use results from time-dependent hydrodynamical simulations of the line-driven wind instability (seeded by the base perturbation) to derive the analytical approximation of X-ray emission in the stellar wind. We use this approximation in our non-LTE wind models and find that an improved inclusion of X-rays leads to a better agreement between model ionization fractions and those derived from observations. Furthermore, the slope of the relation is in better agreement with observations, however the X-ray luminosity is underestimated by a factor of three. We propose a possible solution for this discrepancy.
Key words: stars: winds, outflows / stars: mass-loss / stars: early-type / hydrodynamics / X-rays: stars
© ESO, 2009
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