Abstract: We present an observational analysis of electron cooling/heating rates in the expanding solar wind plasma. Our study is based on a full three component (core-halo-strahl) analytical modeling of measured electron velocity distribution functions. The derived empirical radial profiles of the macroscopic characteristics (i.e. density, temperature and heat flux) are employed to examine properties of theoretical energy balance equations and estimate the required external heating/cooling terms. The complete study is performed for the slow and fast solar wind separately using electron data acquired by Helios 1 and 2 in the heliocentric radial range between 0.3 and 1.0 AU in the ecliptic plane only.

Abstract: We present a novel observation interpreting method for the high-mass X-ray binaries (HMXBs) based on a combination of spectroscopic data and numerical results of a radiation hydrodynamic model of stellar wind in HMXBs. By using an indirect imaging method of Doppler tomography, we calculate synthetic tomograms of a predicted emission in Low/Hard and High/Soft X-ray states and compare them with tomograms produced using phase-resolved optical spectra of Cygnus X-1, a prototype of HMXBs. The emissions of HMXBs are determined by the local conditions within the circumstellar medium - namely by local density, temperature, and ionization parameter. These quantities are computed by the radiation hydrodynamic code and strongly depend on the X-ray state of such 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 a good agreement with the observational data.