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X-Ray Binary (XRB) ○꠹｜Definition｜1st｜20251119205401-00-⌔

X-ray binary - Wikipedia

X-ray binary

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X-ray binaries are a class of binary stars that are luminous in X-rays. The X-rays are produced by matter falling from one component, called the donor (usually a relatively common main sequence star), to the other component, called the accretor, which can be a white dwarf, neutron star or black hole. The infalling matter releases gravitational potential energy, up to 30 percent of its rest mass, as X-rays. (Hydrogen fusion releases only about 0.7 percent of rest mass.) The lifetime and the mass-transfer rate in an X-ray binary depends on the evolutionary status of the donor star, the mass ratio between the stellar components, and their orbital separation.¹

An estimated 10${}^{41}$ positrons escape per second from a typical low-mass X-ray binary.²³

Printed 2026-06-28.

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Footnotes

1. Tauris, Thomas M.; van den Heuvel, Ed (2006). “Chapter 16: Formation and evolution of compact stellar X-ray sources”. In Lewin, Walter; van der Klis, Michiel (eds.). Compact Stellar X-ray Sources. Cambridge Astrophysics Series. Vol. 39. pp. 623–665. arXiv:astro-ph/0303456. Bibcode:2006csxs.book..623T. doi:10.1017/CBO9780511536281.017. ISBN 978-0-521-82659-4. S2CID 18856214. ↩

2. Weidenspointner, Georg (2008). “An asymmetric distribution of positrons in the Galactic disk revealed by gamma-rays”. Nature. 451 (7175): 159–62. Bibcode:2008Natur.451..159W. doi:10.1038/nature06490. PMID 18185581. S2CID 4333175. ↩

3. “Mystery of Antimatter Source Solved – Maybe” by John Borland 2008 ↩

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