GRO J0422+32
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Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
---|---|
Constellation | Perseus |
Right ascension | 04h 21m 42.77s[1] |
Declination | +32° 54′ 26.7″[1] |
Apparent magnitude (V) | 13.2 |
Distance | 7,800[2] ly (2,400 pc) |
Spectral type | M4.5V[1] + Black hole |
Other designations | |
V518 Per, GRO J0422+33, RLC2006 XB2, Granat 0417+335, Nova Persei 1992, Nova Persei 1993, ZGH2005 OS00676-097731
GRO J0422+32, ZGH2005 XS00676B3-003 | |
Database references | |
SIMBAD | data |
GRO J0422+32[1] is an X-ray nova and black hole candidate that was discovered by the BATSE instrument on the CGRO satellite on 5 August 1992.[3][4] During outburst, it was observed to be stronger than the Crab Nebula gamma-ray source out to photon energies of about 500 keV.[2]
The mass of the black hole in GRO J0422+32 falls in the range 3.66 to 4.97 solar masses.[5] This is the smallest yet found for any stellar black hole, and near the theoretical upper mass limit (~2.7 M☉) for a neutron star. Further analysis in 2012 calculated a mass of 2.1 M☉, which raises questions as to what the object actually is.[6]
It is also known to have a companion M-type main-sequence star, V518 Per,[7] in the constellation Perseus. It has a magnitude of 13.5 in the B spectral band, and 13.2 in the visible band.
See also
References
- ^ a b c d "GRO J0422+32". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 4 December 2016.
- ^ a b Ling, J. C.; Wm; Wheaton, A. (2003). "BATSE Soft γ-Ray Observations of GROJ0422+32". Astrophys. J. 584 (1): 399–413. arXiv:astro-ph/0210673. Bibcode:2003ApJ...584..399L. doi:10.1086/345602. S2CID 118954541.
- ^ Harmon, A. et al. (1992) IAUC 5584
- ^ Paciesas, W. et al. (1992), IAUC 5594
- ^ "GRO J0422+32: The Lowest Mass Black Hole?". The Astrophysical Journal. 599 (2): 1254–1259. 2003. arXiv:astro-ph/0308490. Bibcode:2003ApJ...599.1254G. doi:10.1086/379311. S2CID 17785067.
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ignored (help) - ^ Kreidberg, Laura; Bailyn, Charles D.; Farr, Will M.; Kalogera, Vicky (2012). "Mass Measurements of Black Holes in X-ray Transients: is There a Mass Gap?". The Astrophysical Journal. 757 (36): 17pp. arXiv:1205.1805. Bibcode:2012ApJ...757...36K. doi:10.1088/0004-637x/757/1/36. S2CID 118452794.
- ^ General Catalogue of Variable Stars, 3rd ed. (1971) Moscow[page needed]