Physics
Scientific paper
Aug 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996svphu..39..759c&link_type=abstract
Soviet Physics Uspekhi, Vol. 39, No. 8, p. 759 - 780
Physics
9
Black Holes: X-Ray Binaries, Black Holes: Masses
Scientific paper
Mass determination methods and their results for ten black holes in X-ray binary systems are summarised. A unified interpretation of the radial velocity and optical light curves allows to reliably justify the close binary system model and to prove the correctness of determination of the optical star mass function fv(m). The orbit plane inclination i can be estimated from an analysis of the optical light curve of the system, which is due mainly to the ellipsoidal shape of the optical star (the so-called ellipticity effect). The component mass ratio q = mx/mv is obtained from information about the distance to the binary system as well as from data about rotational broadening of absorption lines in the spectrum of the optical star. These data allow to obtain from the value of fv(m) a reliable value of the black hole mass mx or its low limit, as well as the optical star mass mv. An independent estimate of the optical star mass mv obtained from information about its spectral class and luminosity gives test results. Additional test comes from information about the absence or presence of X-ray eclipses in the system. Effects of the non-zero dimension of the optical star, its pear-like shape, and X-ray heating on the absorption line profiles and the radial velocity curve are investigated. It is very significant that none of ten known massive (mx > 3 Msun) X-ray sources considered as black hole candidates is an X-ray pulsar or an X-ray burster of the first kind.
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