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X-ray binary
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{{Short description|Class of binary stars}} [[Image:Accretion disk.jpg|300px|thumb|Artist's impression of an X-ray Binary]] '''X-ray binaries''' are a class of [[binary star]]s that are luminous in [[X-ray]]s. 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 energy|gravitational potential energy]], up to 30 percent of its rest mass, as X-rays. (Hydrogen [[nuclear fusion|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.<ref name=Tauris>{{cite book |first1=Thomas M. |last1=Tauris |first2=Ed |last2=van den Heuvel |title=Compact Stellar X-ray Sources |chapter=Chapter 16: Formation and evolution of compact stellar X-ray sources |bibcode=2006csxs.book..623T |volume=39 |editor1-first=Walter |editor1-last=Lewin |editor2-first=Michiel |editor2-last=van der Klis |series=Cambridge Astrophysics Series |year=2006 |pages=623β665 |doi=10.1017/CBO9780511536281.017 |arxiv=astro-ph/0303456 |isbn=978-0-521-82659-4|s2cid=18856214 }}</ref> An estimated 10<sup>41</sup> [[positron]]s escape per second from a typical [[X-ray binary#Low-mass X-ray binary|low-mass X-ray binary]].<ref>{{Cite journal | last = Weidenspointner | first = Georg | title = An asymmetric distribution of positrons in the Galactic disk revealed by gamma-rays | journal = Nature | date = 2008 | doi = 10.1038/nature06490 |bibcode = 2008Natur.451..159W | pmid=18185581 | volume=451 | issue = 7175 | pages=159β62| s2cid = 4333175 }}</ref><ref>[https://www.wired.com/wiredscience/2008/01/mystery-of-anti/ "Mystery of Antimatter Source Solved β Maybe"] by John Borland 2008</ref>
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