Question: How are X-ray binaries described?
About the article "Black hole", section "X-ray binaries".

Candidate passages:
X-ray binaries are further subdivided into several (sometimes overlapping) subclasses, that perhaps reflect the underlying physics better.
Note that the classification by mass (high, intermediate, low) refers to the optically visible donor, not to the compact X-ray emitting accretor.
Low-mass X-ray binaries (LMXBs) * Soft X-ray transients (SXTs) * Symbiotic X-ray binaries * Super soft X-ray sources or Super soft sources (SSSs),(SSXB)  Intermediate-mass X-ray binaries (IMXBs)  High-mass X-ray binaries (HMXBs) * Be/X-ray binaries (BeXRBs) * Supergiant X-ray binaries (SGXBs) * Supergiant Fast X-ray Transients (SFXTs)  Others * X-ray bursters * X-ray pulsars * Microquasars (radio-jet X-ray binaries that can house either a neutron star or a black hole)  
Mitra is the first astrophysicist to suggest that photo-meson process rather than proton-proton collision process could be the leading mechanism for Ultra High Energy gamma-ray production in ultra-compact X-ray binaries. 
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 plenty of gas in a short time.
As the gas falls onto the neutron star, a bright flare in hard X-rays is seen. 
The Catalog of High-Mass X-ray Binaries in the Galaxy (4th Ed.)
contains source name(s), coordinates, finding charts, X-ray luminosities, system parameters, and stellar parameters of the components and other characteristic properties for 114 HMXBs, together with a comprehensive selection of the relevant literature.
About 60% of the high-mass X-ray binary candidates are known or suspected Be/X-ray binaries, while 32% are supergiant/X-ray binaries (SGXB).
For all the main-sequence and subgiant stars of spectral types A, F, G, and K and luminosity classes IV and V listed in the Bright Star Catalogue (BSC, also known as the HR Catalogue) that have been detected as X-ray sources in the ROSAT All-Sky Survey (RASS), there is the RASSDWARF - RASS A-K Dwarfs/Subgiants Catalog.
The total number of RASS sources amounts to ~150,000 and in the BSC 3054 late-type main-sequence and subgiant stars of which 980 are in the catalog, with a chance coincidence of 2.2% (21.8 of 980). 
There are a growing number of recurrent X-ray transients, characterized by short outbursts with very fast rise times (~ tens of minutes) and typical durations of a few hours that are associated with OB supergiants and hence define a new class of massive X-ray binaries: Supergiant Fast X-ray Transients (SFXTs).
XTE J1739–302 is one of these.
Discovered in 1997, remaining active only one day, with an X-ray spectrum well fitted with a thermal bremsstrahlung (temperature of ∼20 keV), resembling the spectral properties of accreting pulsars, it was at first classified as a peculiar Be/X-ray transient with an unusually short outburst.
A new burst was observed on Apr 8 2008 with Swift.