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WR 93b

From Wikipedia, the free encyclopedia
Wolf-Rayet star in the constellation of Scorpius
WR 93b
Location of WR 93b (circled in red).Scorpius runs across the top of the image fromAntares at top left to the end of the tail on the right.
Observation data
EpochJ2000.0      EquinoxJ2000.0
ConstellationScorpius
Right ascension17h 32m 03.308s[1]
Declination−35° 04′ 32.62″[1]
Apparent magnitude (V)15.2[2]
Characteristics
Evolutionary stageWolf-Rayet star
Spectral typeWO3[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 mas[1]
Distance7,600 ± 500 ly
(2,300 ± 200 pc)
Details
Mass8.1+1.9
−1.2
[6] M
Radius0.44[6] R
Luminosity110,000+53,000
−30,000
[6] L
Temperature160,000[3] K
Other designations
2MASS J17320330-3504323,SSTGLMC G353.2744-00.8460
Database references
SIMBADdata

WR 93b is aWolf-Rayet star in theconstellationScorpius, an extremely rare star on the WO oxygen sequence. It appears nearNGC 6357 in the tail of the scorpion.

Discovery

[edit]

WR 93b was discovered in 2003 during a study of emission line stars from theAAO/UKST Southern Galactic Plane 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 theGalactic Center and is thought to be part of theScutum-Crux spiral arm. It is highly reddened andinterstellar extinction causes it to be 6.5 magnitudes fainter at visual wavelengths than it otherwise would be.[7]

Features

[edit]

WR 93b, ofspectral classification WO3, is one of the very few known oxygen-sequence Wolf-Rayet stars, just four in theMilky Waygalaxy 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 ofthe sun's but with a mass nearly 10 solar masses. Very strongstellar winds, with aterminal velocity of 5,000 kilometers per second are causing WR 93b to lose 10−5 M/year.[3] For comparison, the Sunloses (2-3) x 10−14 solar masses per year due to itssolar wind, several hundred million times less than WR 93b.

Evolutionary status

[edit]

WO Wolf-Rayet stars are the last evolutionary stage of the most massive stars before exploding assupernovae, possibly with agamma-ray burst.[9] It is very likely that WR 93b is on its last stages ofnuclear fusion, near or beyond the end ofhelium burning.[10] It has been calculated that WR 93b will explode as a supernova within 8,000 years.[3]

See also

[edit]

References

[edit]
  1. ^abcdeBrown, A. G. A.; et al. (Gaia collaboration) (2021)."Gaia Early Data Release 3: Summary of the contents and survey properties".Astronomy & Astrophysics.649: A1.arXiv:2012.01533.Bibcode:2021A&A...649A...1G.doi:10.1051/0004-6361/202039657.S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source atVizieR.
  2. ^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. ^abcdTramper, F.; Straal, S. M.; Sanyal, D.; Sana, H.; de Koter, A.; Gräfener, G.; Langer, N.; Vink, J. S.;de Mink, S. E.; Kaper, L. (2015). "Massive stars on the verge of exploding: The properties of oxygen sequence Wolf-Rayet stars".Astronomy & Astrophysics.581 (110): A110.arXiv:1507.00839v1.Bibcode:2015A&A...581A.110T.doi:10.1051/0004-6361/201425390.S2CID 56093231.
  4. ^abcCutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (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.
  5. ^abVan 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.arXiv:astro-ph/0609008.Bibcode:2006A&A...458..453V.doi:10.1051/0004-6361:20065819.S2CID 119104786.
  6. ^abcdSander, 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.arXiv:1201.6354.Bibcode:2012A&A...540A.144S.doi:10.1051/0004-6361/201117830.S2CID 119182468.
  7. ^abDrew, 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.arXiv:astro-ph/0403482.Bibcode:2004MNRAS.351..206D.doi:10.1111/j.1365-2966.2004.07771.x.S2CID 2601618.
  8. ^van der Hucht, Karel A. (2001). "The VIIth catalogue of galactic Wolf–Rayet stars".New Astronomy Reviews.45 (3):135–232.Bibcode:2001NewAR..45..135V.doi:10.1016/S1387-6473(00)00112-3.ISSN 1387-6473.
  9. ^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.arXiv:1308.4681.Bibcode:2013A&A...558A.131G.doi:10.1051/0004-6361/201321906.S2CID 84177572.
  10. ^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.arXiv:1401.7322.Bibcode:2014A&A...564A..30G.doi:10.1051/0004-6361/201322573.S2CID 118870118.
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