Abstract
A large fraction of X-ray sources in our Galaxy are low-mass X-ray binaries, containing a black hole or a neutron star accreting from a gravitationally bound low-mass (\({\lesssim }\)1 M⊙) companion star. These systems are among the older population of stars and accreting systems in the Galaxy and typically have long accretion histories. Low-mass X-ray binaries are categorized into various subclasses based on their observed properties such as X-ray variability and brightness, nature of the companion star and/or the compact object, and binary configuration. In this chapter, we review the phenomenology of subclasses of these systems and summarize observational finding regarding their characteristics, populations, and their distribution in the Galaxy.
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Acknowledgements
The authors thank J. C. A. Miller-Jones, J. M. Corral-Santana, T. J. Maccarone, I. Mandel, J. A. Kennea, K. C. Dage, and K. Auchettl for helpful comments and discussions.
AB is supported by the International Centre for Radio Astronomy Research, a joint venture between Curtin University and the University of Western Australia, funded by the state government of Western Australia and the joint venture partners.
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Bahramian, A., Degenaar, N. (2023). Low-Mass X-ray Binaries. In: Bambi, C., Santangelo, A. (eds) Handbook of X-ray and Gamma-ray Astrophysics. Springer, Singapore. https://doi.org/10.1007/978-981-16-4544-0_94-1
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