Masses of the visual components and black holes in X-ray novae: Effects of proximity of the components


Cite item

Full Text

Open Access Open Access
Restricted Access Access granted
Restricted Access Subscription Access

Abstract

It is shown that the approximation of the complex, tidally distorted shape of a star as a circular disc with local line profiles and a linear limb-darkening law, which is usually applied when deriving equatorial stellar rotation velocities from line profiles, leads to overestimation of the equatorial velocity Vrot sin i and underestimation of the component mass ratio q = Mx/Mv. A formula enabling correction of the effect of these simplifying assumptions on the shape of a star is used to re-determine the mass ratios q and the masses of the black holes Mx and visual components Mv in low-mass X-ray binary systems containing black holes. Taking into account the tidal–rotational distortion of the stellar shape can significantly increase the mass ratios q = Mx/Mv, reducing Mv, while Mx changes only slightly. The resulting distribution of Mv attains its maximum near Mv ≃ 0.35M, in disagreement with the results of population synthesis computations realizing standard models for Galactic X-ray novae with black holes. Possible ways to overcome this inconsistency are discussed. The derived distribution of Mx also differs strongly from the mass distribution for massive stars in the Galaxy.

About the authors

V. S. Petrov

Sternberg Astronomical Institute

Author for correspondence.
Email: patrokl@gmail.com
Russian Federation, Universitetskii pr. 13, Moscow, 119991

E. A. Antokhina

Sternberg Astronomical Institute

Email: patrokl@gmail.com
Russian Federation, Universitetskii pr. 13, Moscow, 119991

A. M. Cherepashchuk

Sternberg Astronomical Institute

Email: patrokl@gmail.com
Russian Federation, Universitetskii pr. 13, Moscow, 119991

Supplementary files

Supplementary Files
Action
1. JATS XML

Copyright (c) 2017 Pleiades Publishing, Ltd.