GRS 1124-683

Today, GRS 1124-683 is a highly relevant topic that captures the attention of people of all ages and backgrounds. Its impact on society and daily life is undeniable, and it generates endless opinions, debates and discussions. It is a topic that arouses curiosity and fascination, but also entails challenges and controversies. In this article, we will explore in detail the different facets of GRS 1124-683, analyzing its influence in various areas, its evolution over time, and the role it plays in people's lives today.

GU Muscae
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Musca
Right ascension 11h 26m 26.60s[1]
Declination −68° 40′ 32.3″[1]
Apparent magnitude (V) 13.3[2]
Spectral typeK3V-K7V[1]
Other designations
GU Mus, GRS 1124-683, 1RXS J112623.5-684040, Nova Muscae 1991
Database references
SIMBADdata

The gamma-ray and X-ray source GRS 1124-683, discovered by the Granat mission and Ginga, is a system containing a black hole candidate. The system also goes by the name X-ray Nova Muscae 1991 or GU Muscae. These two orbiting X-ray telescopes discovered the system when the system produced an outburst of X-rays on January 9, 1991.

Black hole system

A visual band light curve for GU Muscae, adapted from Bailyn (1992)[3]

It is one of several likely black hole systems that are classified as X-ray novae. Such a nova periodically produces bright outbursts of X-rays, along with visible light and other forms of energy.

In such a system, a black hole pulls gas from the surface of a companion star. The gas forms a thin disk around the black hole, known as an accretion disk. In an X-ray nova, the flow of gas is fairly thin and slow, so the accretion disk remains relatively cool, and little gas falls into the black hole.

In the case of GU Muscae, the black hole is about seven times as massive as the Sun, while the companion is three-quarters as massive as the Sun. The companion is also cooler than the Sun, so its surface is redder, and the star's total luminosity is only one-third that of the Sun's. Its outer layers probably were blown away by the supernova explosion that gave birth to the black hole. The two stars orbit each other every 10.4 hours at a distance of roughly 2 million miles (3.2 million km).

Spectral radiance

During the January 20–21, 1991, outburst which led to its discovery, radiation was produced by positron annihilation.[4] The SIGMA telescope aboard GRANAT detected a relatively narrow variable emission line near 500 keV in the spectrum.[4] From January 9 – August 14, 1991, the spectrum had a strong hard component extending up to ~300 keV.[4]

References

  1. ^ a b c "GU Mus". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 8 December 2016.
  2. ^ Liu, Q. Z. (2007). "A catalogue of low-mass X-ray binaries in the Galaxy, LMC, and SMC (Fourth edition)". Astronomy and Astrophysics. 469 (2): 807–810. arXiv:0707.0544. Bibcode:2007A&A...469..807L. doi:10.1051/0004-6361:20077303. S2CID 14673570. Retrieved 7 December 2016.
  3. ^ Bailyn, Charles D. (May 1992). "Periodic Variability in the Optical Counterpart of X-Ray Nova MUSCAE 1991". The Astrophysical Journal. 391: 298–305. Bibcode:1992ApJ...391..298B. doi:10.1086/171346.
  4. ^ a b c Sunyaev R, Churazov E, Gilfanov M, Dyachkov A, Khavenson N, Grebenev S, Kremnev R, Sukhanov K, Goldwurm A, Ballet J, Cordier B, Paul J, Denis M, Vedrenne G, Niel M, Jourdain E (1992). "X-ray nova in Musca (GRS 1124+68): hard X-ray source with narrow annihilation line". Astrophys. J. 389 (2): L75-8. Bibcode:1992ApJ...389L..75S. doi:10.1086/186352.

Harvard website written by Orosz, Jerome A.; Bailyn, Charles D.; McClintock, Jeffrey E.; Remillard, Ronald A.