GRS 1915+105
File:V1487AqlLightCurve.png A near-infrared (K band) light curve for V1487 Aquilae, adapted from Neil et al. (2007)[1] | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Aquila |
| Right ascension | Template:RA[2] |
| Declination | Template:DEC[2] |
| Characteristics | |
| Evolutionary stage | Microquasar[3] |
| Spectral type | KIII[4] |
| Astrometry | |
| Parallax (π) | 0.120±0.009 mas[3] |
| Distance | 28,000 ly (Script error: No such module "val".[3] pc) |
| Details | |
| Black hole | |
| Mass | Script error: No such module "val".[3]Template:Contradiction-inline Template:Solar mass |
| Metallicity [Fe/H] | {{{metal_fe2}}} dex |
| Other designations | |
| V1487 Aquilae, Granat 1915+105, Nova Aquilae 1992, Granat 1915+10, INTEGRAL1 112 | |
| Database references | |
| SIMBAD | data |
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GRS 1915+105 or V1487 Aquilae is an X-ray binary star system containing a main sequence star and a black hole. Transfer of material from the star to the black hole generates a relativistic jet, making this a microquasar system. The jet exhibits apparent superluminal motion.
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 determined by spectroscopic observations.[6]
The binary system lies 11,000 parsecs away[7] in Aquila. The black hole in GRS 1915+105 is 10 to 18 solar masses[8]Template:Contradiction-inline. The black hole rotates at least 950 times per second, giving it a spin parameter >0.82 (1.0 is the theoretical maximum).[9][10]
Galactic superluminal source
In 1994, GRS 1915+105 became the first known galactic source that ejects material with apparent superluminal motion velocities.[11]
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.[12]
See also
References
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External links
- A Very Massive Stellar Black Hole in the Milky Way Galaxy November 28, 2001 (ESO)
- Image V1487 Aquilae
- O maior buraco negro estelar da Via Láctea (The biggest stellar black hole of the Milky Way) - in Portuguese.
- MICRO-QUASAR WITHIN OUR GALAXY
- The micro quasar GRS 1915+105 INTEGRAL Science Data Centre