Editing X-ray binary (section)

== Be star binaries ==
=== Be/X-ray binaries ===
[[Be/X-ray binary|Be/X-ray binaries]] (BeXRBs) are a class of high-mass X-ray binaries that consist of a [[Be star]] and a [[neutron star]]. The neutron star is usually in a wide highly elliptical orbit around the Be star. The Be [[stellar wind]] forms a disk confined to a plane often different from the orbital plane of the neutron star. When the neutron star passes through the Be disk, it accretes a large mass of hot gas in a short time. As the gas falls onto the neutron star, a bright flare in hard X-rays is seen.<ref>{{cite journal|bibcode=2011Ap&SS.332....1R|title=Be/X-ray binaries|journal=Astrophysics and Space Science|volume=332|pages=1–29|last1=Reig|first1=Pablo|year=2011|issue=1 |doi=10.1007/s10509-010-0575-8|arxiv=1101.5036}}</ref>

=== Be–white dwarf X-ray binary systems ===
[[File:A Tale of two stars ESA506449.jpg|thumb|upright=1.5|ESA infographic of BeWD EP J0052 formation, observed by the [[Einstein Probe]]<ref>{{Cite web|url=https://www.esa.int/Science_Exploration/Space_Science/Einstein_Probe_catches_X-ray_odd_couple|title=Einstein Probe catches X-ray odd couple|website=www.esa.int}}</ref>]]
[[Be–white dwarf X-ray binary system]]s (BeWDs) are a rare type of X-ray binary consisting of a [[white dwarf]] that accretes matter from a rapidly-rotating [[Be star]]. These systems form through binary evolution where mass transfer spins up the accretor to become a Be star while the donor evolves into a white dwarf.<ref name=ep>{{cite journal |doi=10.3847/2041-8213/ad9580 |doi-access=free |title=Einstein Probe Discovery of EP J005245.1−722843: A Rare Be–White Dwarf Binary in the Small Magellanic Cloud? |date=2025 |last1=Marino |first1=A. |last2=Yang |first2=H. N. |last3=Coti Zelati |first3=F. |last4=Rea |first4=N. |last5=Guillot |first5=S. |last6=Jaisawal |first6=G. K. |last7=Maitra |first7=C. |last8=Ness |first8=J.-U. |last9=Haberl |first9=F. |last10=Kuulkers |first10=E. |last11=Yuan |first11=W. |last12=Feng |first12=H. |last13=Tao |first13=L. |last14=Jin |first14=C. |last15=Sun |first15=H. |last16=Zhang |first16=W. |last17=Chen |first17=W. |last18=Van Den Heuvel |first18=E. P. J. |last19=Soria |first19=R. |last20=Zhang |first20=B. |last21=Weng |first21=S.-S. |last22=Ji |first22=L. |last23=Zhang |first23=G. B. |last24=Pan |first24=X. |last25=Lv |first25=Z. |last26=Zhang |first26=C. |last27=Ling |first27=Z. X. |last28=Chen |first28=Y. |last29=Jia |first29=S. |last30=Liu |first30=Y. |journal=The Astrophysical Journal Letters |volume=980 |issue=2 |pages=L36 |display-authors=1 }}</ref> Only eight BeWDs are known, though theoretical models say they should be 7 times more common than Be/neutron star binaries.