Editing X-ray binary (section)

== High-mass X-ray binary ==
A '''high-mass X-ray binary''' ('''HMXB''') is a [[binary star]] system that is strong in X rays, and in which the normal stellar component is a massive [[star]]: usually an O or B star, a blue [[supergiant]], or in some cases, a red supergiant or a [[Wolf–Rayet star]]. 
The compact, X-ray emitting, component is a [[neutron star]] or [[black hole]].{{r|Tauris}}
A fraction of the [[stellar wind]] of the massive normal star is captured by the compact object, and produces [[X-ray]]s as it falls onto the compact object.

In a high-mass X-ray binary, the massive star dominates the emission of optical light, while the compact object is the dominant source of X-rays. 
The massive stars are very luminous and therefore easily detected. 
One of the most famous high-mass X-ray binaries is [[Cygnus X-1]], which was the first identified black hole candidate.  
Other HMXBs include [[Vela X-1]] (not to be confused with [[Vela X]]), and [[4U 1700-37]].

The variability of HMXBs are observed in the form of [[X-ray pulsar]]s and not [[X-ray burster]]s. These [[X-ray pulsar]]s are due to the accretion of matter magnetically funneled into the poles of the compact companion.<ref name=":1" /> The [[stellar wind]] and [[Roche lobe]] overflow of the massive normal star accretes in such large quantities, the transfer is very unstable and creates a short lived mass transfer.

Once a HMXB has reached its end, if the periodicity of the binary was less than a year, it can become a single [[Thorne%E2%80%93%C5%BBytkow_object|red giant with a neutron core]] or a single [[neutron star]]. With a longer periodicity, a year and beyond, the HMXB can become a double [[neutron star]] binary if uninterrupted by a [[supernova]].<ref name=":0" />