X-ray emission from hydrodynamical wind simulations in non-LTE models
| Authors | |
|---|---|
| Year of publication | 2011 |
| Type | Article in Proceedings |
| Conference | Active OB stars: structure, evolution, mass loss, and critical limits |
| MU Faculty or unit | |
| Citation | |
| Web | http://adsabs.harvard.edu/abs/2011IAUS..272..614K |
| Doi | http://dx.doi.org/10.1017/S1743921311011562 |
| Field | Astronomy and astrophysics |
| Keywords | stars: winds; outflows; stars: early-type; hydrodynamics; X-rays: stars |
| Description | Massive hot stars are strong sources of X-ray emission originating in their winds. Although hydrodynamical wind 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 crude approximations. To improve this, we use results from time-dependent hydrodynamical simulations of the line-driven wind instability to derive an 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, albeit the X-ray luminosity is underestimated by a factor of three. We propose that a possible solution for this discrepancy is connected with the wind porosity. |
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