X-ray emission from hydrodynamical simulations in non-LTE wind models

J. Krticka1, A. Feldmeier2 L.M. Oskinova2, J. Kubat3, W.-R. Hamann2,

1Ustav teoreticke fyziky a astrofyziky, Masarykova univerzita, Brno, Czech Republic
2Institut für Physik und Astronomie, Universität Potsdam, Germany
3Astronomicky ustav, Akademie ved Ceske republiky, Ondrejov, Czech Republic

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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