X-ray emission from hydrodynamical simulations in non-LTE wind models
J. Krticka1, A. Feldmeier2 L.M. Oskinova2, J. Kubat3, W.-R. Hamann2,
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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