X-ray emission from hydrodynamical simulations in non-LTE wind models
Abstract
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 servations. Furthermore, the slope of the L_x-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.
Cite
@article{arxiv.0910.3430,
title = {X-ray emission from hydrodynamical simulations in non-LTE wind models},
author = {J. Krticka and A. Feldmeier and L. M. Oskinova and J. Kubat and W. -R. Hamann},
journal= {arXiv preprint arXiv:0910.3430},
year = {2015}
}
Comments
9 pages, accepted for publication in Astronomy and Astrophysics