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SMC 018136

Summary

SMC 018136, also known as PMMR 37, is a red supergiant star located in the Small Magellanic Cloud. It is one of the largest stars and one of the most luminous SMC cool supergiants so far discovered, with a radius of 945 times that of the sun and a bolometric luminosity almost 200,000 times more than Sun. If it were in the place of the Sun, its photosphere would at least engulf the orbit of Mars.[6]

SMC 018136

SMC 018136 is visible in the full-size image
Observation data
Epoch J2000      Equinox J2000
Constellation Tucana
Right ascension 0h 50m 56.095s[1]
Declination -72° -15m -6.07s[1]
Apparent magnitude (V) 11.61[2]
Characteristics
Spectral type K4.5 Ia-Ib,[3] M0Ia[4]
Apparent magnitude (K) 7.849±0.020[1]
Astrometry
Radial velocity (Rv)185.7[5] km/s
Details
Radius945[6] R☉
Luminosity186,000[6] L☉
Surface gravity (log g)−0.4[7] cgs
Temperature3,900[6] K
Other designations
TYC 9138-1852-1, 2MASS J00505609-7215060, GSC 09138-01852
Database references
SIMBADdata

SMC 018136 has a spectral type M0 Ia[4] and an effective temperature 3,900 K,[6] although more recent papers suggest it has a slightly earlier spectral type of K4.5 Ia-Ib.[3]

See also edit

References edit

  1. ^ a b c "2MASS". VizieR. Centre de Données astronomiques de Strasbourg. Retrieved 27 March 2017.
  2. ^ Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27. Bibcode:2000A&A...355L..27H.
  3. ^ a b Davies, Ben; Crowther, Paul A.; Beasor, Emma R. (2018). "The luminosities of cool supergiants in the Magellanic Clouds, and the Humphreys–Davidson limit revisited". Monthly Notices of the Royal Astronomical Society. 478 (3): 3138–3148. arXiv:1804.06417. Bibcode:2018MNRAS.478.3138D. doi:10.1093/mnras/sty1302. S2CID 59459492.
  4. ^ a b Humphreys, R. M. (1979). "M supergiants and the low metal abundances in the Small Magellanic Cloud". Astrophysical Journal. 231: 384. Bibcode:1979ApJ...231..384H. doi:10.1086/157201.
  5. ^ González-Fernández, Carlos; Dorda, Ricardo; Negueruela, Ignacio; Marco, Amparo (2015). "A new survey of cool supergiants in the Magellanic Clouds". Astronomy & Astrophysics. 578: A3. arXiv:1504.00003. Bibcode:2015A&A...578A...3G. doi:10.1051/0004-6361/201425362. S2CID 55959019.
  6. ^ a b c d e Massey, Philip; Neugent, Kathryn F.; Ekström, Sylvia; Georgy, Cyril; Meynet, Georges (2023-01-01). "The Time-averaged Mass-loss Rates of Red Supergiants as Revealed by Their Luminosity Functions in M31 and M33". The Astrophysical Journal. 942 (2): 69. arXiv:2211.14147. Bibcode:2023ApJ...942...69M. doi:10.3847/1538-4357/aca665. ISSN 0004-637X.
  7. ^ Dicenzo, Brooke; Levesque, Emily M. (2019). "Atomic Absorption Line Diagnostics for the Physical Properties of Red Supergiants". The Astronomical Journal. 157 (4): 167. arXiv:1902.01862. Bibcode:2019AJ....157..167D. doi:10.3847/1538-3881/ab01cb. S2CID 119076156.