X-ray emission from hydrodynamical simulations in non-LTE wind models
| Authors | |
|---|---|
| Year of publication | 2009 |
| Type | Article in Periodical |
| Magazine / Source | Astronomy and Astrophysics |
| MU Faculty or unit | |
| Citation | |
| Web | http://www.aanda.org/index.php?option=article&access=standard&Itemid=129&url=/articles/aa/abs/2009/47/aa12642-09/aa12642-09.html |
| Field | Astronomy and astrophysics |
| Keywords | stars: winds; outflows -- stars: mass-loss -- stars: early-type -- hydrodynamics -- X-rays: stars |
| Description | 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 LX-L 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. |
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