GS 2000+25 (original) (raw)
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Star in the constellation Vulpecula
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 dataEpoch J2000 Equinox J2000 | |
| Constellation | Vulpecula |
| Right ascension | 20h 02m 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 | |
| Distance | 8800 ± 2300 ly (2700 ± 700[4] pc) |
| Orbit | |
| Period (P) | 8.26 hr[2] |
| Details | |
| Black hole | |
| Mass | 7.2–7.8[3] M☉ |
| Other designations | |
| Nova Vul 1988, INTREF 1007, QZ Vul[5] | |
| Database references | |
| SIMBAD | data |
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.
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]
- ^ 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.