X-ray binary

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Artist's impression of an X-ray Binary Accretion disk.jpg
Artist's impression of an X-ray Binary

X-ray binaries are a class of binary stars that are luminous in X-rays. The X-rays are produced by matter falling from one component, called the donor (usually a relatively common main sequence star), to the other component, called the accretor, which is either a neutron star or black hole. The infalling matter releases gravitational potential energy, up to 30 percent of its rest mass, as X-rays. (Hydrogen fusion releases only about 0.7 percent of rest mass.) The lifetime and the mass-transfer rate in an X-ray binary depends on the evolutionary status of the donor star, the mass ratio between the stellar components, and their orbital separation. [1]

Contents

An estimated 1041 positrons escape per second from a typical low-mass X-ray binary. [2] [3]

Classification

Microquasar SS-433. A game-changer SS-433.tif
Microquasar SS-433.

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 binary

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. [1] 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, [11] and of these, thirteen LMXBs have been discovered in globular clusters. The Chandra X-ray Observatory has revealed LMXBs in many distant galaxies. [12]

A typical low-mass X-ray binary emits almost all of its radiation in X-rays, 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 bursters, but can sometimes be seen in the form of X-ray pulsars. The X-ray bursters are created by thermonuclear explosions created by the accretion of Hydrogen and Helium. [13]

Intermediate-mass X-ray binary

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.

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. [1] A fraction of the stellar wind of the massive normal star is captured by the compact object, and produces X-rays 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 pulsars and not X-ray bursters. These X-ray pulsars are due to the accretion of matter magnetically funneled into the poles of the compact companion. [13] 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 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. [14]

Microquasar

Artist's impression of the microquasar SS 433. Ss433 art big.gif
Artist's impression of the microquasar SS 433.

A microquasar (or radio emitting X-ray binary) is the smaller cousin of a quasar. Microquasars are named after quasars, as they have some common characteristics: strong and variable radio emission, often resolvable as a pair of radio jets, and an accretion disk surrounding a compact object which is either a black hole or a neutron star. In quasars, the black hole is supermassive (millions of solar masses); in microquasars, the mass of the compact object is only a few solar masses. In microquasars, the accreted mass comes from a normal star, and the accretion disk is very luminous in the optical and X-ray regions. Microquasars are sometimes called radio-jet X-ray binaries to distinguish them from other X-ray binaries. A part of the radio emission comes from relativistic jets, often showing apparent superluminal motion. [15]

Microquasars are very important for the study of relativistic jets. The jets are formed close to the compact object, and timescales near the compact object are proportional to the mass of the compact object. Therefore, ordinary quasars take centuries to go through variations a microquasar experiences in one day.

Noteworthy microquasars include SS 433, in which atomic emission lines are visible from both jets; GRS 1915+105, with an especially high jet velocity and the very bright Cygnus X-1, detected up to the High Energy gamma rays (E > 60 MeV). Extremely high energies of particles emitting in the VHE band might be explained by several mechanisms of particle acceleration (see Fermi acceleration and Centrifugal mechanism of acceleration).

See also

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References

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  2. ↑ Weidenspointner, Georg (2008). "An asymmetric distribution of positrons in the Galactic disk revealed by gamma-rays". Nature. 451 (7175): 159–62. Bibcode:2008Natur.451..159W. doi:10.1038/nature06490. PMID   18185581. S2CID   4333175.
  3. ↑ "Mystery of Antimatter Source Solved – Maybe" by John Borland 2008
  4. ↑ "A game-changer". www.eso.org. Retrieved 15 July 2019.
  5. ↑ Introduction to Cataclysmic Variables (CVs), NASA, 2006.
  6. ↑ Patruno, Alessandro; Watts, Anna L. (2021), Belloni, Tomaso M.; Méndez, Mariano; Zhang, Chengmin (eds.), "Accreting Millisecond X-ray Pulsars", Timing Neutron Stars: Pulsations, Oscillations and Explosions, vol. 461, Berlin, Heidelberg: Springer, pp. 143–208, arXiv: 1206.2727 , Bibcode:2021ASSL..461..143P, doi:10.1007/978-3-662-62110-3_4, ISBN   978-3-662-62110-3, S2CID   118471125 , retrieved 2022-06-16
  7. ↑ "Millisecond Pulsar Catalog - Black Sidus". 2013-09-30. Retrieved 2022-06-16.
  8. ↑ Chen, Wen-Cong; Podsiadlowski, Philipp (2016). "Evolution of Intermediate-mass X-Ray Binaries Driven by the Magnetic Braking of AP/BP Stars. I. Ultracompact X-Ray Binaries". The Astrophysical Journal. 830 (2): 131. arXiv: 1608.02088 . Bibcode:2016ApJ...830..131C. doi: 10.3847/0004-637X/830/2/131 . S2CID   118475703.
  9. ↑ Negueruela, I; Smith, D. M; Reig, P; Chaty, S; Torrejón, J. M (2006). "Supergiant Fast X-ray Transients: A New Class of High Mass X-ray Binaries Unveiled by INTEGRAL". The X-Ray Universe 2005. 604 (2006): 165. arXiv: astro-ph/0511088 . Bibcode:2006ESASP.604..165N.
  10. ↑ Sidoli, Lara; Ed van den Heuvel (2008). "Transient outburst mechanisms". 37th COSPAR Scientific Assembly. 37: 2892. arXiv: 0809.3157 . Bibcode:2008cosp...37.2892S.
  11. ↑ Liu, Q. Z; Van Paradijs, J; Van Den Heuvel, E. P. J (2007). "A catalogue of low-mass X-ray binaries in the Galaxy, LMC, and SMC (Fourth edition)". Astronomy and Astrophysics. 469 (2): 807. arXiv: 0707.0544 . Bibcode:2007A&A...469..807L. doi:10.1051/0004-6361:20077303. S2CID   14673570.
  12. ↑ Tetarenko, B. E.; Sivakoff, G. R.; Heinke, C. O.; Gladstone, J. C. (February 10, 2010). "Watchdog: A Comprehensive All-Sky Database of Galactic Black Hole X-Ray Binaries". The Astrophysical Journal Supplement Series. 222 (2): 15. arXiv: 1512.00778 . doi: 10.3847/0067-0049/222/2/15 . S2CID   118833989.
  13. 1 2 3 Tauris, Thomas M; Van Den Heuvel, Edward P. J; Savonije, Gerrit J (2000). "Formation of Millisecond Pulsars with Heavy White Dwarf Companions:Extreme Mass Transfer on Subthermal Timescales". The Astrophysical Journal. 530 (2): L93–L96. arXiv: astro-ph/0001013 . Bibcode:2000ApJ...530L..93T. doi:10.1086/312496. PMID   10655173. S2CID   17772120.
  14. 1 2 Podsiadlowski, Ph; Rappaport, S; Pfahl, E. D (2002). "Evolutionary Sequences for Low- and Intermediate-Mass X-Ray Binaries". The Astrophysical Journal. 565 (2): 1107. arXiv: astro-ph/0107261 . Bibcode:2002ApJ...565.1107P. doi:10.1086/324686. S2CID   16381236.
  15. ↑ Mirabel, I. F.; Rodríguez, L. F. (1994-09-01). "A superluminal source in the Galaxy". Nature. 371 (6492): 46–48. Bibcode:1994Natur.371...46M. doi:10.1038/371046a0. ISSN   0028-0836. S2CID   4347263.
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