SMC 018136: Difference between revisions
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'''SMC |
'''SMC 018136''', also known as '''PMMR 37''', is a [[M-type star|M-type supergiant star]] with a temperature of 3,575 [[Kelvin|K]] and a [[radial velocity]] of 185.7 km/s located in the [[Small Magellanic Cloud]]. |
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==Stellar Properties== |
==Stellar Properties== |
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{{Stars of Tucana}} |
{{Stars of Tucana}} |
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Revision as of 20:57, 7 September 2018
.jpg) SMC 18136 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 | M0Ia[3] |
| Apparent magnitude (K) | 7.849 ± 0.020[1] |
| Astrometry | |
| Radial velocity (Rv) | 185.7[4] km/s |
| Details | |
| Radius | 1,310[5] R☉ |
| Luminosity | 254,000[5] L☉ |
| Temperature | 3,575[5] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
SMC 018136, also known as PMMR 37, is a M-type supergiant star with a temperature of 3,575 K and a radial velocity of 185.7 km/s located in the Small Magellanic Cloud.
Stellar Properties
SMC 018136 is a red supergiant of spectral type M3.5Ia with an effective temperature 3,575 K, a bolometric luminosity over 200,000 times more than Sun, and a radius over 1,300 times wider than the sun, making it one of the largest stars so far discovered. If it were in the place of the Sun, its photosphere would at least engulf the orbit of Jupiter. This would make it the largest star in the Small Magellanic Cloud.
See also
References
- ^ a b c "2MASS". VizieR. Centre de Données astronomiques de Strasbourg. Retrieved 27 March 2017.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ a b c Levesque, E. M.; Massey, P.; Olsen, K. A. G.; Plez, B.; Meynet, G.; Maeder, A. (2006). "The Effective Temperatures and Physical Properties of Magellanic Cloud Red Supergiants: The Effects of Metallicity". The Astrophysical Journal. 645 (2): 1102. arXiv:astro-ph/0603596. Bibcode:2006ApJ...645.1102L. doi:10.1086/504417.
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