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Black-Hole Systems: Optical Spectroscopy and IR Photometry

Published online by Cambridge University Press:  25 May 2016

P.A. Charles
P.A. Charles*
Affiliation:
Oxford University, Nuclear & Astrophysics Laboratory, Keble Road, Oxford 0X1 3RH, United Kingdom

Abstract

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The X-ray transient systems have provided the first opportunities for detailed studies of the mass losing star in low-mass X-ray binaries. During X-ray quiescence the cool star is the dominant light source in the red and near-IR. Optical spectroscopy yields the mass function (itself a lower limit to the compact-object mass), the rotational broadening leads to the mass ratio, q (assuming only that the star fills its Roche lobe), and the IR ellipsoidal light curve gives the system inclination (for high q). In such cases, a complete solution to the system parameters is possible, and this has been performed for A 0620-00 (V616 Mon) and GS 2023+338 (V404 Cyg), leading to the first accurate black-hole masses (which are in the range 10–12 M⊙).

Type
5 X-ray Binaries
Information
Symposium - International Astronomical Union , Volume 165: Compact Stars in Binaries , 1996 , pp. 341 - 350
Copyright
Copyright © Kluwer 1996 

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