GRO J1655-40
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Double star GRO J1655-40 |
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| Artist's impression of GRO J1655-40 | |||
| AladinLite | |||
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Observation dates equinox : J2000.0 , epoch : J2000.0 |
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| Constellation | Scorpio | ||
| Right ascension | 16 h 54 m 0.14 s | ||
| declination | -39 ° 50 ′ 44.9 ″ | ||
| Apparent brightness | 14.0 - 17.3 V mag | ||
| Typing | |||
| B − V color index | 1.0 | ||
| Spectral class | F6III + BH | ||
| Variable star type | LMXB / BHXB / XN + E | ||
| Astrometry | |||
| distance | 10,432 ± 652 Lj 3,200 ± 200 pc |
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| Proper movement | |||
| Rec. Share: | 0.1 ± 10.0 mas / a | ||
| Dec. portion: | -8.5 ± 9.8 mas / a | ||
| Physical Properties | |||
| Dimensions | (7.0 / 2.34) M ☉ | ||
| Rotation time | 2.62083 d | ||
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Other names and catalog entries |
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GRO J1655-40 is referred to as L ow M ass X -ray B inary ( LMXB , dt. Ray binary system with a small mass) denotes that of a developed under Tallstar the spectral F6III with about two and a half times the mass of the sun and a stellar black hole of the seven times the mass Sun, whichorbit each other once every 2.6 daysin the constellation Scorpio .
Together with Cygnus X-1 , GRO J1655-40 is one of ten known galactic microquasars (as of 2019).
The distance from our solar system is about 3,200 pc or 10,500 ly . GRO J1655-40 and his companion move at a speed of 112 km / s in a strongly eccentric galactic orbit (e = 0.34 ± 0.05) through the Milky Way . The black hole was formed at a distance of more than 3 kpc from the galactic center and must have been shot into such an eccentric orbit by the explosion of the precursor star. The linear momentum and the kinetic energy of this BHXB (Black Hole X-ray binary) are comparable to those of solitary neutron stars and millisecond pulsars . GRO J1655-40 is the first black hole for which there is evidence that this high escape velocity was transmitted by a supernova explosion when it was formed.
The X-ray spectrum of this binary star system shows that turbulent winds of several million degrees of hot gas swirl around the black hole. Much of the hot gas travels inward towards the black hole, but about 30% is blown away.
The temperature and intensity of the winds require that strong magnetic fields be present. These magnetic fields create magnetic turbulence that causes friction in the accretion disk and drive winds from the disk that carry angular momentum outward as the gas falls inward. Magnetic friction also heats up the gas in the inner part of the disk so much that it emits X-rays.
Individual evidence
- ↑ a b c d V1033 Sco. In: SIMBAD . Center de Données astronomiques de Strasbourg , accessed June 28, 2019 .
- ↑ a b c d V1033 Sco. In: VSX. AAVSO , accessed June 28, 2019 .
- ↑ Optical Observations of GRO J1655-40 in Quiescence. I. A Precise Mass for the Black Hole Primary. In: Jerome A. Orosz, et al. The Astrophysical Journal, Volume 477, Number 2, accessed July 1, 2019 .
- ↑ a b GRO J1655-40: NASA's Chandra Answers Black Hole Paradox. In: NASA . Harvard-Smithsonian Center for Astrophysics , accessed July 1, 2019 .