Astronomy:WR 111
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Sagittarius |
| Right ascension | 18h 08m 28.46870s[1] |
| Declination | −21° 15′ 11.1844″[1] |
| Apparent magnitude (V) | +7.82[2] |
| Characteristics | |
| Evolutionary stage | Wolf-Rayet[3] |
| Spectral type | WC5[3] |
| U−B color index | −0.38[2] |
| B−V color index | −0.28[2] |
| Astrometry | |
| Proper motion (μ) | RA: 0.293±0.129[4] mas/yr Dec.: −1.527±0.107[4] mas/yr |
| Parallax (π) | 0.5826 ± 0.0759[4] mas |
| Distance | 1,630+320 −230[5] pc |
| Absolute magnitude (MV) | −4.26[6] |
| Details | |
| Semi-empirical model | |
| Mass | 13.0[6] M☉ |
| Radius | 1.99[6] R☉ |
| Luminosity | 245,000[6] L☉ |
| Temperature | 89,000[6] K |
| Hydrodynamical model | |
| Mass | 13.63[7] M☉ |
| Radius | 0.905[7] R☉ |
| Luminosity | 282,000[7] L☉ |
| Temperature | 140,000[7] K |
| Age | 4.2[8] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
WR 111 (HD 165763) is a Wolf-Rayet (WR) star in the constellation Sagittarius. It is magnitude 7.8 and lies about 5,150 light-years away. It is one of the brightest and most closely studied WR stars.
History
In 1880, Edward Pickering reported that BD−21°4864 had a spectrum similar to a nova, but it was apparently a non-variable star that had been near 8th magnitude since at least 1849.[9] It was included in Campbell's 1894 paper The Wolf-Rayet stars.[10]
In the Henry Draper Catalogue, BD−21°4864 was listed as entry 165763 with a spectral type of Oa. It was described in 1925 as a "Be star" due to its very strong emission lines,[11] and in 1927 as a class-O star with unusually broad emission features.[12] After the classification of WR stars onto either the nitrogen or carbon sequence, HD 165763 was designated as WC6 and its temperature estimated from the strength of Ov and Civ emission.[13]
In 1968, the WR spectral classes were revised and HD 165763 was used as an example of class WC5. In this catalogue, considered as the fifth catalogue of Wolf Rayet stars, it was designated MR 84.[14] In the sixth WR catalogue, the current naming convention was adopted and this star was numbered as WR 111.[15]
Location
WR 111 is one of the 20 brightest Wolf Rayet stars in the sky.[16] It lies in a rich Milky Way field near to V4381 Sagittarii and HD 165516, but not apparently a member of the associated cluster.[17]
Properties
WR 111 is considered an archetypal WC5 star, having dominant emission lines of Civ, plus strong Ciii emission as well as Oiii, Oiv, and Ov, but not Ovi.[6]
Non-hydrodynamical atmospheric models calculate a "surface" temperature of 89,000 K. The surface in this context is defined as the depth in the atmosphere at which the optical depth reaches 20. This differs from the convention used for many types of star, due to the optically dense stellar winds of WR stars. The corresponding radius is at 2.10 R☉.[6] A more detailed individual study of WR 111 using a hydrodynamical atmospheric model gives a temperature of 140,000 K and a radius of 0.905 R☉.[7] The apparently large difference is due largely to a difference in the depth within the atmosphere at which the radius is defined.[6] The luminosity of WR 111 is similar in both models at 245,000 L☉ - 282,000 L☉, and the masses are found to be 13.0 M☉ and 13.83 M☉, respectively.[7][6]
The stellar wind from WR 111 is ejecting 20 millionths of the Sun's mass every year at a speed of 2,398 km/s.[6] The mechanism driving the intense stellar wind is found to be an opacity bump deep within the atmosphere caused by highly ionised iron. The winds are then accelerated to high velocity in the outer atmosphere by less highly ionised iron and by carbon and oxygen.[7]
References
- ↑ 1.0 1.1 van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V.
- ↑ 2.0 2.1 2.2 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues 2237: 0. Bibcode: 2002yCat.2237....0D.
- ↑ 3.0 3.1 Michaux, Yannick J. L.; Moffat, Anthony F. J.; Chené, André-Nicolas; St-Louis, Nicole (2014). "On the origin of variable structures in the winds of hot luminous stars". Monthly Notices of the Royal Astronomical Society 440 (1): 2–9. doi:10.1093/mnras/stt2102. Bibcode: 2014MNRAS.440....2M.
- ↑ 4.0 4.1 4.2 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 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. doi:10.1093/mnras/stz3614. Bibcode: 2020MNRAS.493.1512R.
- ↑ 6.0 6.1 6.2 6.3 6.4 6.5 6.6 6.7 6.8 6.9 Sander, A.; Hamann, W.-R.; Todt, H. (2012). "The Galactic WC stars. Stellar parameters from spectral analyses indicate a new evolutionary sequence". Astronomy & Astrophysics 540: A144. doi:10.1051/0004-6361/201117830. Bibcode: 2012A&A...540A.144S.
- ↑ 7.0 7.1 7.2 7.3 7.4 7.5 7.6 Gräfener, G.; Hamann, W.-R. (2005). "Hydrodynamic model atmospheres for WR stars. Self-consistent modeling of a WC star wind". Astronomy and Astrophysics 432 (2): 633. doi:10.1051/0004-6361:20041732. Bibcode: 2005A&A...432..633G.
- ↑ Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (2011). "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society 410 (1): 190–200. doi:10.1111/j.1365-2966.2010.17434.x. Bibcode: 2011MNRAS.410..190T.
- ↑ Pickering, Edward C. (1880). "Novel Celestial Object". Nature 22 (569): 483. doi:10.1038/022483c0. Bibcode: 1880Natur..22..483P. https://zenodo.org/record/1429249.
- ↑ Campbell, W. W. (1894). "The Wolf-Rayet stars". Astronomy and Astro-Physics 13: 448. Bibcode: 1894AstAp..13..448C.
- ↑ Merrill, P. W.; Humason, M. L.; Burwell, C. G. (1925). "Discovery and Observations of Stars of Class Be". Astrophysical Journal 61: 389. doi:10.1086/142899. Bibcode: 1925ApJ....61..389M.
- ↑ Payne, Cecilia H. (1927). "Spectroscopic Energy Diagrams for Five Stars of Class O". Harvard College Observatory Bulletin 844: 17. Bibcode: 1927BHarO.844...17P.
- ↑ Beals, C. S. (1940). "On the Physical Characteristics of the Wolf Rayet Stars and their Relation to Other Objects of Early Type (with Plates VIII, IX)". Journal of the Royal Astronomical Society of Canada 34: 169. Bibcode: 1940JRASC..34..169B.
- ↑ Smith, Lindsey F. (1968). "A revised spectral classification system and a new catalogue for galactic Wolf-Rayet stars". Monthly Notices of the Royal Astronomical Society 138: 109–121. doi:10.1093/mnras/138.1.109. Bibcode: 1968MNRAS.138..109S.
- ↑ Van Der Hucht, K. A.; Conti, P. S.; Lundstrom, I.; Stenholm, B. (1981). "The Sixth Catalogue of galactic Wolf-Rayet stars, their past and present". Space Science Reviews 28 (3): 227. doi:10.1007/BF00173260. Bibcode: 1981SSRv...28..227V.
- ↑ Van Der Hucht, Karel A. (2001). "The VIIth catalogue of galactic Wolf-Rayet stars". New Astronomy Reviews 45 (3): 135–232. doi:10.1016/S1387-6473(00)00112-3. Bibcode: 2001NewAR..45..135V.
- ↑ Kharchenko, N. V.; Piskunov, A. E.; Schilbach, E.; Röser, S.; Scholz, R.-D. (2013). "Global survey of star clusters in the Milky Way. II. The catalogue of basic parameters". Astronomy & Astrophysics 558: A53. doi:10.1051/0004-6361/201322302. Bibcode: 2013A&A...558A..53K.
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