WOH G17

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WOH G17
Observation data
Epoch J2000      Equinox
Constellation Mensa
Right ascension 04h 39m 23.671s[1]
Declination −73° 11′ 02.68″[1]
Apparent magnitude (V) 13.8[2]
Characteristics
Evolutionary stage RSG or AGB[3]
Spectral type M[4]
Apparent magnitude (K) 5.52
Apparent magnitude (G) 11.15
Apparent magnitude (H) 5.59
Apparent magnitude (J) 6.92
Variable type LPV (Mira or SR)[1]
Astrometry
Radial velocity (Rv)101.213[5] km/s
Proper motion (μ) RA: 2.159[1] mas/yr
Dec.: 7.138[1] mas/yr
Parallax (π)0.0116 ± 0.0875[1] mas
Details
Luminosity4,000[3] L☉
Surface gravity (log g)+0.5?[6] cgs
Temperature3,328[1] K
Other designations
WOH G17, IRAS 04403-7316, 2MASS J04392369-7311028, LMC 1150
Database references
SIMBADdata

WOH G17 is a possible red supergiant (RSG) located in the Large Magellanic Cloud (LMC) or a Mira variable asymptotic giant branch (AGB) star[3] in the constellation of Mensa. The star is often considered to be a foreground object; much closer than the LMC, probably in the Milky Way, and therefore is potentially much smaller and less luminous.[6]

As a red supergiant, it would be one of the largest known stars, with a luminosity of 933,000 L☉ and temperature of 3,300 K implying a radius of about 2,955 solar radii (2.056×109 km; 13.74 au),[6] which is somewhat on par with the largest red supergiants known. This would correspond to a volume 25.8 billion times bigger than the Sun. If placed at the center of the Solar system its photosphere would engulf the orbit of Saturn and reach to about 3/4 the distance to Uranus’s orbit.

See also[]

References[]

  1. ^ a b c d e f g 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. ^ 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. ^ a b c Kastner, Joel H.; Thorndike, Stephen L.; Romanczyk, Paul A.; Buchanan, Catherine L.; Hrivnak, Bruce J.; Sahai, Raghvendra; Egan, Michael (2008). "The Large Magellanic Cloud's Top 250: Classification of the Most Luminous Compact 8 μm Sources in the Large Magellanic Cloud". The Astronomical Journal. 136 (3): 1221–1241. arXiv:astro-ph/0703584. Bibcode:2008AJ....136.1221K. doi:10.1088/0004-6256/136/3/1221. S2CID 117820349.
  4. ^ Westerlund, B. E.; Olander, N.; Hedin, B. (1981). "Supergiant and giant M type stars in the Large Magellanic Cloud". Astronomy and Astrophysics Supplement Series. 43: 267. Bibcode:1981A&AS...43..267W.
  5. ^ Kordopatis, G.; Gilmore, G.; Steinmetz, M.; Boeche, C.; Seabroke, G. M.; Siebert, A.; Zwitter, T.; Binney, J.; De Laverny, P.; Recio-Blanco, A.; Williams, M. E. K.; Piffl, T.; Enke, H.; Roeser, S.; Bijaoui, A.; Wyse, R. F. G.; Freeman, K.; Munari, U.; Carrillo, I.; Anguiano, B.; Burton, D.; Campbell, R.; Cass, C. J. P.; Fiegert, K.; Hartley, M.; Parker, Q. A.; Reid, W.; Ritter, A.; Russell, K. S.; et al. (2013). "The Radial Velocity Experiment (RAVE): Fourth Data Release". The Astronomical Journal. 146 (5): 134. arXiv:1309.4284. Bibcode:2013AJ....146..134K. doi:10.1088/0004-6256/146/5/134. S2CID 119221010.
  6. ^ a b c Groenewegen, Martin A. T.; Sloan, Greg C. (2018). "Luminosities and mass-loss rates of Local Group AGB stars and Red Supergiants". Astronomy & Astrophysics. 609: A114. arXiv:1711.07803. Bibcode:2018A&A...609A.114G. doi:10.1051/0004-6361/201731089. ISSN 0004-6361. S2CID 59327105.
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