SMC 018136
.jpg) 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 | -73° 44m 53.93s[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 | |
| Radius | 945[6] R☉ |
| Luminosity | 186,000[6] L☉ |
| Surface gravity (log g) | −0.4[7] cgs |
| Temperature | 3,900[6] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
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 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]
- ↑ 1.0 1.1 1.2 "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.
- ↑ 3.0 3.1 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. Unknown parameter
|s2cid=ignored (help) - ↑ 4.0 4.1 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. Unknown parameter
|s2cid=ignored (help) - ↑ 6.0 6.1 6.2 6.3 6.4 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.
- ↑ 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. Unknown parameter
|s2cid=ignored (help)
 | This supergiant-related article is a stub. You can help EverybodyWiki by expanding it. |
This article "SMC 018136" is from Wikipedia. The list of its authors can be seen in its historical and/or the page Edithistory:SMC 018136. Articles copied from Draft Namespace on Wikipedia could be seen on the Draft Namespace of Wikipedia and not main one.
