WR 120
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Scutum |
| Right ascension | 18h 41m 00.86698s[1] |
| Declination | −4° 26′ 14.47345″[1] |
| Apparent magnitude (V) | 11.93 |
| Characteristics | |
| Evolutionary stage | Wolf-Rayet |
| Spectral type | WN7w[2] |
| U−B color index | 0.13[3] |
| B−V color index | 1.04[3] |
| Astrometry | |
| Parallax (π) | 0.6369 ± 0.1552 mas[1] |
| Distance | 1,500+640 −360[4] pc |
| Absolute magnitude (MV) | −3.81[2] |
| Details | |
| Mass | 7[2] M☉ |
| Radius | 3.78[2] R☉ |
| Luminosity | 83,200[2] L☉ |
| Temperature | 50,100[2] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
WR 120 is a Wolf-Rayet star in the constellation of Scutum, around 4,900 light years away. It is a hydrogen-free weak-lined WN7 star, and is a possible member of the cluster Dolidze 33.[5] From our point of view, WR 120 is reddened by 4.82 magnitudes.[4]
Properties
Analysis of WR 120's spectrum with PoWR shows that it has a temperature of around 50,000 Kelvins, and is losing mass at a rate of 10×10−4.9 M☉/year, or 1 solar mass every 80,000 years, which is being carried away from the surface at a speed of 1,225 kilometres per second.[2] Taking its close distance into account, WR 120's luminosity turns out to be a mere 83,200 L☉, which would make it one of the dimmest WN stars known, and one of the only WN stars with a luminosity below 100,000 L☉. Using the Stefan-Boltzmann Law, a radius of 3.78 R☉ is derived, and a "transformed" radius at an optical depth of 2/3, more comparable to other types of stars, is at about 6 R☉. Using the WR Luminosity-Mass ratio, WR 120 may have a mass of just 7 M☉, one of the lowest masses of any WR star.[2]
WR 120 may be further away than just 1,500 pc from the Sun, as the distance measurement for the cluster of which it may be a member of, Dolidze 33, sits at nearly 3,000 pc.[5]
References
- ^ a b c Gaia Collaboration (2018-04-01). "VizieR Online Data Catalog: Gaia DR2 (Gaia Collaboration, 2018)". VizieR Online Data Catalog. 1345. Bibcode:2018yCat.1345....0G.
- ^ a b c d e f g h Hamann, W.-R.; Gräfener, G.; Liermann, A.; Hainich, R.; Sander, A. A. C.; Shenar, T.; Ramachandran, V.; Todt, H.; Oskinova, L. M. (2019-05-01). "The Galactic WN stars revisited. Impact of Gaia distances on fundamental stellar parameters". Astronomy and Astrophysics. 625: A57. arXiv:1904.04687. Bibcode:2019A&A...625A..57H. doi:10.1051/0004-6361/201834850. ISSN 0004-6361.
- ^ a b 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.
- ^ a b Crowther, Paul A.; Rate, Gemma (2020). "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. S2CID 209444955.
{{cite journal}}: CS1 maint: unflagged free DOI (link) - ^ a b Rate, Gemma; Crowther, Paul A.; Parker, Richard J. (2020-06-01). "Unlocking Galactic Wolf-Rayet stars with Gaia DR2 - II. Cluster and association membership". Monthly Notices of the Royal Astronomical Society. 495: 1209–1226. Bibcode:2020MNRAS.495.1209R. doi:10.1093/mnras/staa1290. ISSN 0035-8711.
{{cite journal}}: CS1 maint: unflagged free DOI (link)
