Abstract This paper is the third in our series of papers devoted to the investigation of X-ray emission from OB stars. In our two previous papers, we study the high-resolution X-ray spectra of 32 O stars and 25 B stars to investigate the correlations between the properties of X-ray emission and stellar parameters. We checked if the X-ray hardness and post-shock plasma temperature grow with increasing stellar magnetic field, mass loss rate and terminal wind velocity. Our previous analysis of high-resolution spectra showed that the correlations are weak or even absent. In the present paper, we analyzed low-resolution X-ray spectra, using model-independent X-ray hardness values for checking the above mentioned dependencies. We establish that X-ray luminosities LX weakly depend on the stellar magnetic field. At the same time, \(L_{\rm X} \propto \dot{M}^{0.5}\) and \(L_{\rm X} \propto E^{0.5}_{\rm kin}\), where \(\dot{M}\) is the mass loss rate and \(E_{\rm kin}\) is the kinetic energy of the wind. The X-ray luminosities decrease with growing magnetic confinement parameter η. We also argue that there is an additional (probably non-thermal) component contributed to the stellar X-ray emission.
Keywords stars: early-type — stars: spectra: X-Ray
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