Astronomy:WR 93b
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Scorpius |
| Right ascension | 17h 32m 03.308s[1] |
| Declination | −35° 04′ 32.62″[1] |
| Apparent magnitude (V) | 15.2[2] |
| Characteristics | |
| Evolutionary stage | Wolf-Rayet star |
| Spectral type | WO3[3] |
| Apparent magnitude (B) | 16.9[4] |
| Apparent magnitude (R) | 14.4[4] |
| Apparent magnitude (J) | 11.331[4] |
| Apparent magnitude (K) | 10.17[5] |
| Astrometry | |
| Proper motion (μ) | RA: −0.642±0.032[1] mas/yr Dec.: −2.1055±0.024[1] mas/yr |
| Parallax (π) | 0.4298 ± 0.0288[1] mas |
| Distance | 7,600 ± 500 ly (2,300 ± 200 pc) |
| Details | |
| Mass | 8.1+1.9 −1.2[6] M☉ |
| Radius | 0.44[6] R☉ |
| Luminosity | 110,000+53,000 −30,000[6] L☉ |
| Temperature | 160,000[3] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
WR 93b is a Wolf-Rayet star in the constellation Scorpius, an extremely rare star on the WO oxygen sequence. It appears near NGC 6357 in the tail of the scorpion.
Discovery
WR 93b was discovered in 2003 during a study of emission line stars from the AAO/UKST Southern Galactic Plane Hα Survey. It was published as the fourth galactic WO class star in 1994.[7] This was too late to be included in the VIIth Wolf Rayet catalogue,[8] but it is listed in an annex published in 2006.[5]
It lies in the direction of the Galactic Center and is thought to be part of the Scutum-Crux spiral arm. It is highly reddened and interstellar extinction causes it to be 6.5 magnitudes fainter at visual wavelengths than it otherwise would be.[7]
Features
WR 93b, of spectral classification WO3, is one of the very few known oxygen-sequence Wolf-Rayet stars, just four in the Milky Way galaxy and six in external galaxies. Modelling the atmosphere gives a luminosity around 110,000 L☉, very low for a Wolf-Rayet star.[6] It is a very small dense star, with a radius less than half of the sun's but with a mass nearly 10 solar masses. Very strong stellar winds, with a terminal velocity of 5,000 kilometers per second are causing WR 93b to lose 10−5 M☉/year.[3] For comparison, the Sun loses (2-3) x 10−14 solar masses per year due to its solar wind, several hundred million times less than WR 93b.
Evolutionary status
WO Wolf-Rayet stars are the last evolutionary stage of the most massive stars before exploding as supernovae, possibly with a gamma-ray burst.[9] It is very likely that WR 93b is on its last stages of nuclear fusion, near or beyond the end of helium burning.[10] It has been calculated that WR 93b will explode as a supernova within 8,000 years.[3]
See also
References
- ↑ 1.0 1.1 1.2 1.3 1.4 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G. Gaia EDR3 record for this source at VizieR.
- ↑ Henden, Arne A.; Levine, Stephen; Terrell, Dirk; Welch, Douglas L. (2015). "APASS - the Latest Data Release". American Astronomical Society Meeting Abstracts #225 225: 336.16. Bibcode: 2015AAS...22533616H.
- ↑ 3.0 3.1 3.2 3.3 Tramper, F.; Straal, S. M.; Sanyal, D.; Sana, H.; de Koter, A.; Gräfener, G.; Langer, N.; Vink, J. S. et al. (2015). "Massive stars on the verge of exploding: The properties of oxygen sequence Wolf-Rayet stars". Astronomy & Astrophysics 581 (110): A110. doi:10.1051/0004-6361/201425390. Bibcode: 2015A&A...581A.110T.
- ↑ 4.0 4.1 4.2 Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E. et al. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues 2246: II/246. Bibcode: 2003yCat.2246....0C. http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=II/246.
- ↑ 5.0 5.1 Van Der Hucht, K. A. (2006). "New Galactic Wolf-Rayet stars, and candidates. An annex to the VIIth Catalogue of Galactic Wolf-Rayet Stars". Astronomy and Astrophysics 458 (2): 453–459. doi:10.1051/0004-6361:20065819. Bibcode: 2006A&A...458..453V.
- ↑ 6.0 6.1 6.2 6.3 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 Drew, Janet E.; Barlow, M. J.; Unruh, Y. C.; Parker, Q. A.; Wesson, R.; Pierce, M. J.; Masheder, M. R. W.; Phillipps, S. (2004). "Discovery of a WO star in the Scutum-Crux arm of the inner Galaxy". Monthly Notices of the Royal Astronomical Society 351 (1): 206–214. doi:10.1111/j.1365-2966.2004.07771.x. Bibcode: 2004MNRAS.351..206D.
- ↑ 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. ISSN 1387-6473. Bibcode: 2001NewAR..45..135V.
- ↑ Groh, Jose H.; Meynet, Georges; Georgy, Cyril; Ekstrom, Sylvia (2013). "Fundamental properties of core-collapse Supernova and GRB progenitors: Predicting the look of massive stars before death". Astronomy & Astrophysics 558: A131. doi:10.1051/0004-6361/201321906. Bibcode: 2013A&A...558A.131G.
- ↑ Groh, Jose (2014). "The evolution of massive stars and their spectra I. A non-rotating 60 Msun star from the zero-age main sequence to the pre-supernova stage". Astronomy & Astrophysics 564: A30. doi:10.1051/0004-6361/201322573. Bibcode: 2014A&A...564A..30G.
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