WR 102ea
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| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Sagittarius |
| Right ascension | 17h 43m 05s |
| Declination | −28° 48′ 30″ |
| Characteristics | |
| Evolutionary stage | Wolf Rayet |
| Spectral type | WN9h[1] |
| Apparent magnitude (K) | 8.8[2] |
| Astrometry | |
| Radial velocity (Rv) | 116 km/s |
| Distance | 26k[1] ly (8k[1] pc) |
| Details | |
| Mass | 58[3] M☉ |
| Radius | 86[1] R☉ |
| Luminosity | 2.5 × 106[1] L☉ |
| Temperature | 25,100[1] K |
| Age | probably 4 × 106 years |
| Other designations | |
FMM 241, qF 241, (erroneously QPM-241), Q10, MGM 5-10, LHO 71 | |
| Database references | |
| SIMBAD | data |
WR 102ea is a Wolf–Rayet star in the Sagittarius constellation. It is the second brightest star in the Quintuplet cluster after WR 102hb. With a luminosity of 2,500,000 times solar, it is also one of the most luminous stars known. Despite the high luminosity it can only be observed at infra-red wavelengths due to the dimming effect of intervening dust on visual light.
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Liermann, A.; Hamann, W. -R.; Oskinova, L. M.; Todt, H.; Butler, K. (2010). "The Quintuplet cluster". Astronomy & Astrophysics 524: A82. arXiv:1011.5796. Bibcode:2010A&A...524A..82L. doi:10.1051/0004-6361/200912612.
- ↑ Liermann, A.; Hamann, W. -R.; Oskinova, L. M. (2009). "The Quintuplet cluster". Astronomy and Astrophysics 494 (3): 1137. arXiv:0809.5199. Bibcode:2009A&A...494.1137L. doi:10.1051/0004-6361:200810371.
- ↑ Adriane Liermann et all (2011). "High-mass stars in the Galactic center Quintuplet cluster". Bulletin de la Societe Royale des Sciences de Liege 80: 160-164.
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