GRO J1719-24

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GRO J1719-24
Observation data
Epoch J2000      Equinox J2000
Constellation Ophiuchus
Right ascension  17h 19m 37s[citation needed]
Declination −25° 01′ 03″[citation needed]
Apparent magnitude (V) 16.65[citation needed]
Distance8500[citation needed] ly
(2600[citation needed] pc)
Absolute magnitude (MV)≥6[1]
Database references

GRO J1719-24 (GRS 1716-249, V2293 Oph, X-Ray Nova Ophiuchi 1993) is supposed to be a low-mass X-ray binary.[1] Its name derives from an X-ray transient, detected in 1993.[2] The system consists of a black hole candidate and a low mass companion, estimated to be a main sequence star of the spectral type K05-V.[3]

The rotation period is uncertain, estimated at 14.7h.[4] The light curve possibly exhibits some faster fluctuations as well, which are hypothesized to be produced by blobs of matter in the accretion disk.[4]


  1. ^ a b Della Valle, M.; Mirabel, I.F.; Rodriguez, L.F. (1994), "The optical and radio counterpart of the X-ray Nova Ophiuchi 1993", Astronomy and Astrophysics, 290: 803, Bibcode:1994A&A...290..803D
  2. ^ Ballet, J.; Denis, M.; Gilfanov, M.; R., Sunyaev (1993), IAU Circ., 5874
  3. ^ Chaty, S.; Mirabel, I. F.; Goldoni, P.; Mereghetti, S.; Duc, P.-A.; Martí, J.; Mignani, R. P. (2002), "Near-infrared observations of Galactic black hole candidates", MNRAS, 331 (4): 1065–1071, arXiv:astro-ph/0112329, Bibcode:2002MNRAS.331.1065C, doi:10.1046/j.1365-8711.2002.05267.x
  4. ^ a b Masetti, N.; Bianchini, A.; Bonibaker, J.; della Valle, M.; Vio, R. (1996), "The superhump phenomenon in GRS 1716-249 (=X-Ray Nova Ophiuchi 1993)", Astronomy and Astrophysics, 314