Low-Mass X-ray Binaries
Arash Bahramian (International Centre for Radio Astronomy Research),, Nathalie Degenaar (Anton Pannekoek Institute for Astronomy)
TL;DR
This paper reviews low-mass X-ray binaries, focusing on their classifications, observational properties, population distribution, and significance as older accreting systems in our Galaxy.
Contribution
It provides a comprehensive overview of the phenomenology, classifications, and observational findings related to low-mass X-ray binaries in the Galaxy.
Findings
Classification based on X-ray variability and brightness
Distribution of systems in the Galaxy
Characteristics of different sub-classes
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 (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 sub-classes 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 sub-classes of these systems and summarize observational finding regarding their characteristics, populations, and their distribution in the Galaxy.
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