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An intermediate-mass X-ray binary (IMXB) is a binary star system where one of the components is a neutron star or a black hole. The other component is an intermediate-mass star. [13] [14] An intermediate-mass X-ray binary is the origin for Low-mass X-ray binary systems.
3XMM J004232.1+411314 is a low-mass X-ray binary hosted in the galaxy M31. It is the most luminous source of hard X-rays in the Andromeda Galaxy. It is also the most luminous source known that shows dips in the X-ray light curve. [1] The compact object in this system has been unambiguously identified as a neutron star with a spin period of 3 ...
X-ray luminosities of 10 33-10 38 erg/s; Deep nitrogen (0.67 keV) and oxygen (0.87 keV) absorption edges in X-ray spectra; The white dwarfs in these systems tend to be massive (0.9-1.35 M ☉) with surface temperatures of 20,000-40,000 K. [4] Detection is challenging as the white dwarf is often embedded within the Be star's decretion disk ...
Probably the best known example of an X-ray binary is the high-mass X-ray binary Cygnus X-1. In Cygnus X-1, the mass of the unseen companion is estimated to be about nine times that of the Sun, [32] far exceeding the Tolman–Oppenheimer–Volkoff limit for the maximum theoretical mass of a neutron star. It is therefore believed to be a black ...
GRS 1915+105 or V1487 Aquilae is an X-ray binary star system containing a main sequence star and a black hole. Transfer of material from the star to the black hole generates a relativistic jet, making this a microquasar system. The jet exhibits apparent superluminal motion.
Vela X-1 is a pulsing, eclipsing high-mass X-ray binary (HMXB) system, associated with the Uhuru source 4U 0900-40 and the supergiant star HD 77581. The X-ray emission of the neutron star is caused by the capture and accretion of matter from the stellar wind of the supergiant companion. Vela X-1 is the prototypical detached HMXB.
Be/X-ray binaries belong to the high-mass X-ray binary category. The optical companion is a non-supergiant, fast-rotating Be type star with emission lines indicating luminosity class III-V. Most BeXRBs have eccentric orbits and contain a neutron star, confirmed through X-ray pulsations. [2] BeXRBs are classified as either transient or persistent.
Her X-1 is the prototype for the massive X-ray binaries although it falls on the borderline, ~2 M ☉, between high- and low-mass X-ray binaries. [2] An intermediate-mass X-ray binary (IMXB) is a binary star system where one of the components is a neutron star or a black hole. The other component is an intermediate mass star. [3]