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Contents

   



(Top)
  


1 Properties  




2 See also  




3 References  













GS 2000+25






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From Wikipedia, the free encyclopedia
  

GS 2000+25


Near-infrared (I band) light curves for QZ Vulpeculae, adapted from Chevalier and Ilovaisky (1993).[1] The data were collected over a 10 night period in July 1991. Data collected on different nights are plotted with different colors. The shape of the light curve changed over a period of approximately two days, leading to different shapes on even or odd numbered days.

Observation data
Epoch J2000      Equinox J2000
Constellation Vulpecula
Right ascension 20h02m 49.58s[2]
Declination +25° 14′ 11.3″[2]
Apparent magnitude (V) 18.2[2]
Characteristics
Spectral type Black hole + K3-6 V[3]
Astrometry
Distance8800 ± 2300 ly
(2700 ± 700[4] pc)
Orbit
Period (P)8.26 hr[2]
Details
Black hole
Mass7.2–7.8[3] M☉
Other designations

Nova Vul 1988, INTREF 1007, QZ Vul[5]

Database references
SIMBADdata

GS 2000+25 is an X-ray binary system in the constellation Vulpecula, consisting of a late K-type star and a black hole. It is also an X-ray nova.

Properties[edit]

Because the black hole is more massive than the companion star, it is the primary of the system. The black hole has a mass of about 5 solar masses while the companion has a mass of about 0.5 solar masses. Because the companion star has a low mass, the system is a low-mass X-ray binary.[6]

See also[edit]

References[edit]

  1. ^ Chevalier, C.; Ilovaisky, S. A. (March 1993). "Optical studies of transient low-mass X-ray binaries. IV. A 10-hour distorsion wave in the quiescent light curve of GS 2000+25". Astronomy and Astrophysics. 269: 301–309. Bibcode:1993A&A...269..301C. Retrieved 28 May 2022.
  • ^ a b c d 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 & Astrophysics. 469 (2): 807. arXiv:0707.0544. Bibcode:2007A&A...469..807L. doi:10.1051/0004-6361:20077303. S2CID 14673570.
  • ^ a b Yungelson, L; Lasota, J.-P (2008). "Evolution of low-mass binaries with black-hole components". New Astronomy Reviews. 51 (10–12): 860–868. arXiv:0801.3433. Bibcode:2008NewAR..51..860Y. doi:10.1016/j.newar.2008.03.017. S2CID 11830754.
  • ^ Reynolds, Mark T; Callanan, Paul J; Robinson, Edward L; Froning, Cynthia S (2008). "Infrared contamination in Galactic X-ray novae". Monthly Notices of the Royal Astronomical Society. 387 (2): 788. arXiv:0804.0370. Bibcode:2008MNRAS.387..788R. doi:10.1111/j.1365-2966.2008.13272.x. S2CID 16918671.
  • ^ "GS 2000+25". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 26 November 2017.
  • ^ Filippenko, Alexei V.; Matheson, Thomas; Barth, Aaron J. (1995). "A Black Hole in the X-Ray Nova GS 2000+25". Astrophysical Journal Letters. 455 (2): L139. Bibcode:1995ApJ...455L.139F. doi:10.1086/309831. S2CID 123161764.


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    • Retrieved from "https://en.wikipedia.org/w/index.php?title=GS_2000%2B25&oldid=1170034255"
    Categories: 
    ●Vulpecula
     ●Objects with variable star designations
     ●Stellar black holes
     ●K-type main-sequence stars
     ●Novae
     ●X-ray binaries
     ●Variable star stubs
     ●Multiple star stubs
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