fbpx
Wikipedia

X-ray binary

December 20, 2023

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 normal 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]

Artist's impression of an X-ray Binary

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

Classification edit

 
Microquasar SS-433.[4]

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 edit

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 edit

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 edit

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 edit

 
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 edit

References edit

  1. ^ a b c Tauris, Thomas M.; van den Heuvel, Ed (2006). "Chapter 16: Formation and evolution of compact stellar X-ray sources". In Lewin, Walter; van der Klis, Michiel (eds.). Compact Stellar X-ray Sources. Cambridge Astrophysics Series. Vol. 39. pp. 623–665. arXiv:astro-ph/0303456. Bibcode:2006csxs.book..623T. doi:10.1017/CBO9780511536281.017. ISBN 978-0-521-82659-4. S2CID 18856214.
  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, Berlin, Heidelberg: Springer, vol. 461, 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. ^ a b c 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. ^ a b 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.

External links edit

  • Negueruela, Ignacio; Torrejon, Jose Miguel; Reig, Pablo; Ribo, Marc; Smith, David M. (2008). Supergiant Fast X-ray Transients and Other Wind Accretors. A Population Explosion: The Nature & Evolution of X-Ray Binaries in Diverse Environments. Vol. 1010. pp. 252–256. arXiv:0801.3863. Bibcode:2008AIPC.1010..252N. doi:10.1063/1.2945052. S2CID 18941968. doi:10.1063/1.2945052 Bibcode:2008AIPC.1010..252N
  • Audio Cain/Gay (2009) Astronomy Cast episode 135: X-ray Astronomy
  • Ultraluminous X-ray Pulsar (ULXP) Catalogue

December 20, 2023
binary, binaries, class, binary, stars, that, luminous, rays, rays, produced, matter, falling, from, component, called, donor, usually, relatively, normal, star, other, component, called, accretor, which, either, neutron, star, black, hole, infalling, matter, . 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 normal 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 Artist s impression of an X ray BinaryAn estimated 1041 positrons escape per second from a typical low mass X ray binary 2 3 Contents 1 Classification 2 Low mass X ray binary 3 Intermediate mass X ray binary 4 High mass X ray binary 5 Microquasar 6 See also 7 References 8 External linksClassification edit nbsp Microquasar SS 433 4 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 5 SSXs SSXB Accreting millisecond X ray pulsars AMXPs 6 7 Intermediate mass X ray binaries IMXBs Ultracompact X ray binaries UCXBs 8 High mass X ray binaries HMXBs Be X ray binaries BeXRBs Supergiant X ray binaries SGXBs Supergiant Fast X ray Transients SFXTs 9 10 Others X ray bursters X ray pulsars Microquasars radio jet X ray binaries that can house either a neutron star or a black hole Low mass X ray binary editA 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 editAn 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 editA 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 edit nbsp 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 gt 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 edit4U 0614 091 LS I 61 303 SS 433 QuasarReferences edit a b c Tauris Thomas M van den Heuvel Ed 2006 Chapter 16 Formation and evolution of compact stellar X ray sources In Lewin Walter van der Klis Michiel eds Compact Stellar X ray Sources Cambridge Astrophysics Series Vol 39 pp 623 665 arXiv astro ph 0303456 Bibcode 2006csxs book 623T doi 10 1017 CBO9780511536281 017 ISBN 978 0 521 82659 4 S2CID 18856214 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 Mystery of Antimatter Source Solved Maybe by John Borland 2008 A game changer www eso org Retrieved 15 July 2019 Introduction to Cataclysmic Variables CVs NASA 2006 Patruno Alessandro Watts Anna L 2021 Belloni Tomaso M Mendez Mariano Zhang Chengmin eds Accreting Millisecond X ray Pulsars Timing Neutron Stars Pulsations Oscillations and Explosions Berlin Heidelberg Springer vol 461 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 Millisecond Pulsar Catalog Black Sidus 2013 09 30 Retrieved 2022 06 16 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 Negueruela I Smith D M Reig P Chaty S Torrejon 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 Sidoli Lara Ed van den Heuvel 2008 Transient outburst mechanisms 37th Cospar Scientific Assembly 37 2892 arXiv 0809 3157 Bibcode 2008cosp 37 2892S 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 amp A 469 807L doi 10 1051 0004 6361 20077303 S2CID 14673570 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 a b c 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 a b 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 Mirabel I F Rodriguez 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 External links editNegueruela Ignacio Torrejon Jose Miguel Reig Pablo Ribo Marc Smith David M 2008 Supergiant Fast X ray Transients and Other Wind Accretors A Population Explosion The Nature amp Evolution of X Ray Binaries in Diverse Environments Vol 1010 pp 252 256 arXiv 0801 3863 Bibcode 2008AIPC 1010 252N doi 10 1063 1 2945052 S2CID 18941968 doi 10 1063 1 2945052 Bibcode 2008AIPC 1010 252N Audio Cain Gay 2009 Astronomy Cast episode 135 X ray Astronomy Ultraluminous X ray Pulsar ULXP Catalogue Retrieved from https en wikipedia org w index php title X ray binary amp oldid 1172047053 Low mass X ray binary, wikipedia, wiki, book, books, library,

article

, read, download, free, free download, mp3, video, mp4, 3gp, jpg, jpeg, gif, png, picture, music, song, movie, book, game, games.