Astronomy:GRS 1915+105

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Short description: Binary system in the constellation Aquila
GRS 1915+105
V1487AqlLightCurve.png
A near-infrared (K band) light curve for V1487 Aquilae, adapted from Neil et al. (2007)[1]
Observation data
Equinox J2000.0]] (ICRS)
Constellation Aquila
Right ascension  19h 15m 11.6s[2]
Declination +10° 56′ 44″[2]
Characteristics
Evolutionary stage Microquasar[3]
Spectral type KIII[4]
Astrometry
Parallax (π)0.120 ± 0.009[3] mas
Distance28,000 ly
(8,600+2,000
−1,600[3] pc)
Details
Black hole
Mass12.4+2.0
−1.8[3] M☉
Other designations
V1487 Aquilae, Granat 1915+105, Nova Aquilae 1992, Granat 1915+10, INTEGRAL1 112
Database references
SIMBADdata

GRS 1915+105 or V1487 Aquilae is an X-ray binary star system which features a regular star and a black hole. It was discovered on August 15, 1992 by the WATCH all-sky monitor aboard Granat.[5] "GRS" stands for "GRANAT source", "1915" is the right ascension (19 hours and 15 minutes) and "105" reflects the approximate declination (10 degrees and 56 arcminutes). The near-infrared counterpart was confirmed by spectroscopic observations.[6] The binary system lies 11,000 parsecs away[7] in Aquila. GRS 1915+105 is the heaviest of the stellar black holes so far known in the Milky Way Galaxy,[8] with 10 to 18 times the mass of the Sun.[9] It is also a microquasar, and it appears that the black hole rotates at least 950 times per second, close to the maximum of 1,150 times per second, with a spin parameter value between 0.82 and 1.00 (maximum possible value).[10][11]

Galactic superluminal source

A sequence of MERLIN observation of the X-ray binary GRS 1915+105 taken over a few days.

In 1994, GRS 1915+105 became the first known galactic source that ejects material with apparent superluminal motion velocities.[12]

Observations with high resolution radio telescopes such as VLA, MERLIN, and VLBI show a bi-polar outflow of charged particles, which emit synchrotron radiation at radio frequencies. These studies have shown that the apparent superluminal motion is due to a relativistic effect known as relativistic aberration, where the intrinsic velocity of ejecta is actually about 90% the speed of light.[7]

Growth regulation

Repeat observations by the Chandra X-Ray Observatory over the period of a decade have revealed what may be a mechanism for self-regulation of the rate of growth of GRS 1915+105. The jet of materials being ejected is occasionally choked off by a hot wind blowing off the accretion disk. The wind deprives the jet of materials needed to sustain it. When the wind dies down, the jet returns.[13]

See also

References

  1. ↑ Neil, Ethan T.; Bailyn, Charles D.; Cobb, Bethany E. (March 2007). "Infrared Monitoring of the Microquasar GRS 1915+105: Detection of Orbital and Superhump Signatures". The Astrophysical Journal 657 (1): 409–414. doi:10.1086/510287. Bibcode: 2007ApJ...657..409N. 
  2. ↑ 2.0 2.1 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. doi:10.1051/0004-6361:20077303. Bibcode: 2007A&A...469..807L. 
  3. ↑ 3.0 3.1 3.2 3.3 Reid, M. J; McClintock, J. E; Steiner, J. F; Steeghs, D; Remillard, R. A; Dhawan, V; Narayan, R (2014). "A Parallax Distance to the Microquasar GRS 1915+105 and a Revised Estimate of its Black Hole Mass". The Astrophysical Journal 796 (1): 2. doi:10.1088/0004-637X/796/1/2. Bibcode: 2014ApJ...796....2R. 
  4. ↑ Abubekerov, M. K; Antokhina, E. A; Cherepashchuk, A. M; Shimanskii, V. V (2006). "The mass of the compact object in the low-mass X-ray binary 2S 0921-630". Astronomy Reports 50 (7): 544. doi:10.1134/S1063772906070043. Bibcode: 2006ARep...50..544A. 
  5. ↑ Castro-Tirado, A. J; Brandt, S; Lund, N (1992). "Grs 1915+105". IAU Circ 5590: 2. Bibcode: 1992IAUC.5590....2C. 
  6. ↑ Castro-Tirado, A. J; Geballe, T. R; Lund, N (1996). "Infrared Spectroscopy of the Superluminal Galactic Source GRS 1915+105 During the September 1994 Outburst". Astrophysical Journal Letters 461 (2): L99. doi:10.1086/310009. Bibcode: 1996ApJ...461L..99C. 
  7. ↑ 7.0 7.1 Fender, R. P; Garrington, S. T; McKay, D. J; Muxlow, T. W. B; Pooley, G. G; Spencer, R. E; Stirling, A. M; Waltman, E. B (1999). "MERLIN observations of relativistic ejections from GRS 1915+105". Monthly Notices of the Royal Astronomical Society 304 (4): 865. doi:10.1046/j.1365-8711.1999.02364.x. Bibcode: 1999MNRAS.304..865F. 
  8. ↑ "A Very Massive Stellar Black Hole in the Milky Way Galaxy". https://www.eso.org/public/news/eso0135/. 
  9. ↑ Greiner, J. (2001). "GRS 1915+105". arXiv:astro-ph/0111540.
  10. ↑ Jeffrey E. McClintock; Rebecca Shafee; Ramesh Narayan; Ronald A. Remillard; Shane W. Davis; Li-Xin Li (2006). "The Spin of the Near-Extreme Kerr Black Hole GRS 1915+105". Astrophysical Journal 652 (1): 518–539. doi:10.1086/508457. Bibcode: 2006ApJ...652..518M. https://iopscience.iop.org/article/10.1086/508457. 
  11. ↑ Jeanna Bryne. "Pushing the Limit: Black Hole Spins at Phenomenal Rate". space.com. https://www.space.com/3141-pushing-limit-black-hole-spins-phenomenal-rate.html. 
  12. ↑ Mirabel, I. F; Rodríguez, L. F (1994). "A superluminal source in the Galaxy". Nature 371 (6492): 46. doi:10.1038/371046a0. Bibcode: 1994Natur.371...46M. 
  13. ↑ "An Erratic Black Hole Regulates Itself" (Press release). NASA. 2009-03-25. Archived from the original on 2017-07-09. Retrieved 2009-04-16.

External links

Coordinates: Sky map 19h 15m 11.6s, +10° 56′ 44″



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