WR 150

Last updated
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  mas [1]
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.

Related Research Articles

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WR 120 is a binary containing two Wolf-Rayet stars in the constellation of Scutum, around 10,000 light years away. The primary is a hydrogen-free weak-lined WN7 star, the secondary is a hydrogen-free WN3 or 4 star, and the system is a possible member of the cluster Dolidze 33. From our point of view, WR 120 is reddened by 4.82 magnitudes, and it has the variable designation of V462 Scuti.

BAT99-7 is a WN-type Wolf-Rayet star located in the Large Magellanic Cloud, in the constellation of Dorado, about 160,000 light years away. The star has a spectrum containing extremely broad emission lines, and is the prototype for the "round line" stars, Wolf-Rayet stars whose spectra are characterized by strong and broad emission lines with round line profiles. The broad emission lines hint at an extremely high temperature of nearly 160,000 Kelvin, which would make it the hottest of all WN stars with known temperatures, as well as an extraordinarily large mass loss rate for a Wolf-Rayet star in the LMC, at 10−4.48 M☉/yr, which means that every 30,200 years, the star loses 1 solar mass worth of mass.

References

  1. 1 2 3 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. 1 2 3 4 5 6 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. S2CID   67754788.
  3. ↑ 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.
  4. ↑ 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: 1512–1529. Bibcode:2020MNRAS.493.1512R. doi:10.1093/mnras/stz3614. ISSN   0035-8711.
  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. doi:10.1051/0004-6361/201833712. ISSN   0004-6361.
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