  We present a novel method for interpreting observations of high-mass X-ray
binaries (HMXBs) based on a combination of spectroscopic data and numerical
results from a radiation hydrodynamic model of stellar winds. We calculate
synthetic Doppler tomograms of predicted emission in low/hard and high/soft
X-ray states and compare them with Doppler tomograms produced using spectra of
Cygnus X-1, a prototype of HMXBs. Emission from HMXBs is determined by local
conditions within the circumstellar medium, namely density, temperature, and
ionization state. These quantities depend strongly on the X-ray state of the
systems. By increasing intensity of an X-ray emission produced by the compact
companion in the HMXB model, we achieved a complete redistribution of the
circumstellar medium in the vicinity of the modelled system. These changes
(which simulate the transitions between two major spectral states) are also
apparent in the synthetic Doppler tomograms which are in good agreement with
the observations.

Solar and Stellar Astrophysics;High Energy Astrophysical Phenomena