Editing X-ray binary (section)

== Low-mass X-ray binary ==
[[File:X-Ray binary.jpg|thumb|Artist's impression of an X-ray binary system]]
A '''low-mass X-ray binary''' ('''LMXB''') is a [[binary star]] system where one of the components is either a [[black hole]] or [[neutron star]].{{r|Tauris}}  The other component, a donor, usually fills its [[Roche lobe]] and therefore transfers mass to the compact star.  In LMXB systems the donor is less massive than the compact object, and can be on the [[main sequence]], a degenerate dwarf ([[white dwarf]]), or an evolved star ([[red giant]]). Approximately two hundred LMXBs have been detected in the [[Milky Way]],<ref>{{Cite journal |arxiv = 0707.0544|bibcode = 2007A&A...469..807L|title = A catalogue of low-mass X-ray binaries in the Galaxy, LMC, and SMC (Fourth edition)|journal = Astronomy and Astrophysics|volume = 469|issue = 2|pages = 807|last1 = Liu|first1 = Q. Z|last2 = Van Paradijs|first2 = J|last3 = Van Den Heuvel|first3 = E. P. J|year = 2007|doi = 10.1051/0004-6361:20077303|s2cid = 14673570}}</ref> and of these, thirteen LMXBs have been discovered in [[globular cluster]]s.  The [[Chandra X-ray Observatory]] has revealed LMXBs in many distant galaxies. <ref>{{cite journal | last1=Tetarenko  | first1=B. E. | last2=Sivakoff | first2=G. R. | last3=Heinke | first3=C. O. | last4=Gladstone | first4=J. C. | title=Watchdog: A Comprehensive All-Sky Database of Galactic Black Hole X-Ray Binaries | date= February 10, 2010 | journal= The Astrophysical Journal Supplement Series | volume= 222 | issue= 2 | page=15 | doi=10.3847/0067-0049/222/2/15| arxiv=1512.00778 | s2cid=118833989 | doi-access=free }}</ref>

A typical low-mass X-ray binary emits almost all of its [[electromagnetic radiation|radiation]] in [[X-ray]]s, and typically less than one percent in visible light, so they are among the brightest objects in the X-ray sky, but relatively faint in visible light. The [[apparent magnitude]] is typically around 15 to 20. The brightest part of the system is the [[accretion disk]] around the compact object. The orbital periods of LMXBs range from ten minutes to hundreds of days.

The variability of LMXBs are most commonly observed as [[X-ray burster]]s, but can sometimes be seen in the form of [[X-ray pulsar]]s. The [[X-ray burster]]s are created by [[thermonuclear explosion]]s created by the accretion of Hydrogen and Helium.<ref name=":1" />