WR 150
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Cygnus |
| Right ascension | 21h 50m 05.57248s[1] |
| Declination | +50° 42′ 24.7151″[1] |
| Apparent magnitude (V) | 13.47 |
| Characteristics | |
| Evolutionary stage | Wolf-Rayet |
| Spectral type | WC5[2] |
| B−V color index | 0.53[3] |
| Astrometry | |
| Parallax (π) | 0.024 ± 0.0255[1] mas |
| Distance | 8,730+1,700 −1,380[4] pc |
| Absolute magnitude (MV) | −5.26[2] |
| Details | |
| Mass | 24.8[2] M☉ |
| Radius | 3.59[2] R☉ |
| Luminosity | 724,000[2] L☉ |
| Temperature | 89,000[2] K |
| Other designations | |
2MASS J21500557+5042247 | |
| Database references | |
| SIMBAD | data |
WR 150 is a Wolf-Rayet star in the constellation of Cygnus. It is one of the early-type carbon sequence (WCE), and is of spectral type WC5. WR 150 is very far from the Earth, being 28,500 light-years from it.
Properties
Wolf-Rayet stars are extremely hot stars, and WR 150 is no exception, and is even hotter than most Wolf-Rayet stars. WR 150 has a temperature approaching 90,000 K, similar to WR 111. However unlike WR 111, WR 150 is more than 3 times more luminous than it. As a result, intrinsically, WR 150 is a full magnitude brighter than WR 111. [5]
WR 150 loses mass much more quickly than almost any WC star. It loses 10−4.19 M☉ (about 6.46×10−5 M☉) a year, on a strong stellar wind with a terminal velocity of 3,000 kilometres per second. This means that in 50,000 years, WR 150 will have lost around 3.2 solar masses.
References
- ↑ 1.0 1.1 1.2 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Sander, A. A. C.; Hamann, W.-R.; Todt, H.; Hainich, R.; Shenar, T.; Ramachandran, V.; Oskinova, L. M. (2019-01-01). "The Galactic WC and WO stars. The impact of revised distances from Gaia DR2 and their role as massive black hole progenitors". Astronomy and Astrophysics. 621: A92. arXiv:1807.04293. Bibcode:2019A&A...621A..92S. doi:10.1051/0004-6361/201833712. ISSN 0004-6361. Unknown parameter
|s2cid=ignored (help) - ↑ Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". VizieR Online Data Catalog. 2237. Bibcode:2002yCat.2237....0D.
- ↑ Rate, Gemma; Crowther, Paul A. (2020-03-01). "Unlocking Galactic Wolf-Rayet stars with Gaia DR2 - I. Distances and absolute magnitudes". Monthly Notices of the Royal Astronomical Society. 493 (1): 1512–1529. arXiv:1912.10125. Bibcode:2020MNRAS.493.1512R. doi:10.1093/mnras/stz3614. ISSN 0035-8711.
- ↑ Sander, A. A. C.; Hamann, W.-R.; Todt, H.; Hainich, R.; Shenar, T.; Ramachandran, V.; Oskinova, L. M. (2019-01-01). "The Galactic WC and WO stars. The impact of revised distances from Gaia DR2 and their role as massive black hole progenitors". Astronomy and Astrophysics. 621: A92. arXiv:1807.04293. Bibcode:2019A&A...621A..92S. doi:10.1051/0004-6361/201833712. ISSN 0004-6361. Unknown parameter
|s2cid=ignored (help)
This article "WR 150" is from Wikipedia. The list of its authors can be seen in its historical and/or the page Edithistory:WR 150. Articles copied from Draft Namespace on Wikipedia could be seen on the Draft Namespace of Wikipedia and not main one.
