Abstract
While X-ray observatories continue to identify black-hole candidates on the basis of specific characteristics (such as X-ray spectrum and fast temporal variability), it is necessary to undertake optical spectroscopic dynamical studies of these objects in order to unequivocally show that they could not be (conventional) neutron stars. Such work has expanded dramatically in recent years as a result of the discovery of ~20 soft X-ray transients whose extended periods of X-ray quiescence provide an ideal opportunity for ground-based studies of the mass-losing star in these close interacting binaries. Mass functions have now been derived for eight of these systems that, combined with ellipsoidal studies to constrain the orbital inclinations, imply they significantly exceed the canonical maximum neutron star mass of 3M⊙. They therefore represent the most secure dynamically determined black hole candidates in our Galaxy.
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Charles, P. (1999). Black Holes in Our Galaxy. In: Chakrabarti, S.K. (eds) Observational Evidence for Black Holes in the Universe. Astrophysics and Space Science Library, vol 234. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-4750-7_20
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DOI: https://doi.org/10.1007/978-94-011-4750-7_20
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