V766 Centauri
V766 Centauri | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Centaurus |
| Right ascension | 13h47m10.867s |
| Declination | -62°35′22.96″ |
| Apparent magnitude (V) | 6.1 - 7.5[1] |
| Characteristics | |
| Spectral type | K0 0-Ia[2] |
| B−V color index | +1.98 |
| Variable type | irregular |
| Astrometry | |
| Radial velocity (Rv) | −38.20 km/s |
| Proper motion (μ) | RA: −2.94 mas/yr Dec.: −-2.54 mas/yr |
| Parallax (π) | 1.35 ± 1.59 mas |
| Distance | 3,600[1] pc |
| Details | |
| Mass | 39 (combined)[1] M☉ |
| Radius | 1,315[1] R☉ |
| Luminosity | ~500,000-1,000,000[1] L☉ |
| Surface gravity (log g) | 0[1] cgs |
| Temperature | ~5,000[1] K |
| Rotation | 10-30[1] |
| Other designations | |
| Database references | |
| SIMBAD | data |
V766 Centauri (V766 Cen) is a yellow hypergiant star in the constellation Centaurus. The spectral type is variable around G8Ia+ - K3Ia+[1] and the brightness varies in an irregular fashion. It has a distant B-type companion and is in close contact with a cool companion.[1] It is around 3,600 parsecs from Earth and is the largest known yellow hypergiant, most likely due to interactions with the close companion.
This type of star has evolved from an initial mass of around 40 times the sun to a red hypergiant and is now shedding its remaining outer layers in a series of dramatic explosions, progressively increasing in temperature. It may become a blue supergiant or luminous blue variable before declining in luminosity as a late type Wolf–Rayet star, but is expected to explode as a supernova before that point.
The very high luminosity, extreme size, and mass exchange with the lower mass companion make this an unusual star within a very rare class of starts, but it has been relatively poorly studied until recently.[1]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 1.10 Chesneau, O.; Meilland, A.; Chapellier, E.; Millour, F.; Van Genderen, A. M.; Nazé, Y.; Smith, N.; Spang, A. et al. (2014). "The yellow hypergiant HR 5171 A: Resolving a massive interacting binary in the common envelope phase". arXiv:1401.2628v2 [astro-ph.SR].
- ↑ Keenan, P. C.; McNeil, R. C. (1989). "The Perkins catalog of revised MK types for the cooler stars". The Astrophysical Journal Supplement Series 71: 245. doi:10.1086/191373.
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