V838 Monocerotis
Star in the constellation Monoceros / From Wikipedia, the free encyclopedia
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V838 Monocerotis (Nova Monocerotis 2002) is a spectroscopic binary star system in the constellation Monoceros about 19,000 light years (6 kpc) from the Sun. The previously unremarked star was observed in early 2002 experiencing a major outburst, and was one of the largest known stars for a short period following the outburst.[10] Originally believed to be a typical nova eruption, it was then identified as the first of a new class of eruptive variables known as luminous red novae. The reason for the outburst is still uncertain, but is thought to have been a merger of two stars within a triple system.
Hubble Space Telescope image of V838 Monocerotis and the surrounding nebula on September 9, 2006 Credit: NASA/ESA | |
Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Monoceros |
Right ascension | 07h 04m 04.822s[1] |
Declination | −03° 50′ 50.53″[1] |
Apparent magnitude (V) | 6.75 (2002), 15.6[2] |
Characteristics | |
Evolutionary stage | M-type supergiant[3] |
Spectral type | M7.5I -> M5.5I + B3V[3] |
Variable type | LRN[3] |
Astrometry | |
Proper motion (μ) | RA: −0.536±0.229[4] mas/yr Dec.: −0.078±0.174[4] mas/yr |
Parallax (π) | 0.163 ± 0.016 mas[5] |
Distance | 19,200 ly (5,900±400[6] pc) |
Details | |
Mass | 5 – 10[7] M☉ |
Radius | 467[8] R☉ |
Luminosity | 23,000[8] L☉ |
Temperature | 3,300[8] K |
Age | 4[9] Myr |
Other designations | |
Database references | |
SIMBAD | data |
The eruption occurred on one of two B3 main sequence stars in a close binary orbit. The erupting star appeared as an unusually cool supergiant and for a while engulfed its companion. By 2009 the temperature of the supergiant had increased (since 2005) to 3,270 K and its luminosity was 15,000 times solar (L☉), but its radius had decreased to 380 times that of the Sun (R☉), although the ejecta continues to expand.[11]