WOH S264
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| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Dorado (LMC) |
| Right ascension | 05h 24m 19.3095s[1] |
| Declination | −69° 38′ 49.374″[1] |
| Apparent magnitude (V) | 14.271[2] |
| Characteristics | |
| Evolutionary stage | Red supergiant |
| Spectral type | M3 I[3] |
| Apparent magnitude (U) | 19.519[4] |
| Apparent magnitude (B) | 16.688[4] |
| Apparent magnitude (R) | 11[4] |
| Apparent magnitude (G) | 12.135779[5] |
| Apparent magnitude (I) | 10.804[4] |
| Apparent magnitude (J) | 8.36[4] |
| Apparent magnitude (H) | 7.375[4] |
| Apparent magnitude (K) | 6.809[4] |
| Astrometry | |
| Radial velocity (Rv) | 263.49±1.02[6] km/s |
| Parallax (π) | 0.0457 ± 0.027[5] mas |
| Distance | 45,590[7] pc |
| Details | |
| Mass | 24.9[8] M☉ |
| Radius | 1,390+130 −110[3] R☉ |
| Luminosity | 282,000+49,300 −42,000[3] L☉ |
| Surface gravity (log g) | +0.5±0.1[3] cgs |
| Temperature | 3,570+59 −46[3] K |
| Other designations | |
WOH S264, LI-LMC 976, MSX LMC 461, RM 1-339, SP77 47-10[1] | |
| Database references | |
| SIMBAD | data |
WOH S264 ([W60] B90) is a large, highly luminous[3] red supergiant star in the Large Magellanic Cloud.
Discovery[edit]
WOH S264 was discovered in 1956 by Karl Gordon Henize in a catalogue of H-alpha emission stars and nebulae in the Large Magellanic Cloud. He designated it LHA 120-N 132E, indicating emission line nebula 132E on plate 120. The LHA is originally LHα, standing for H-alpha emission objects identified at the Lamont-Hussey Observatory.[9]
The designation WOH S264 indicates that it is supergiant 264 in a 1981 survey by Westerlund, Olander, and Hedin.[10]
Properties[edit]
WOH S264 is believed to be one of the largest, most luminous red supergiants in the Large Magellanic Cloud with a luminosity of more than 280,000 solar luminosities and a radius of around 1,390 solar radii.[3] It needs further investigation to constrain the luminosity and radius with higher certainty.[3]
See also[edit]
References[edit]
- ↑ 1.0 1.1 1.2 "[W60] B90". Université de Strasbourg.
- ↑ Ulaczyk, K.; Szymański, M. K.; Udalski, A.; Kubiak, M.; Pietrzyński, G.; Soszyński, I.; Wyrzykowski, Ł.; Poleski, R.; Gieren, W.; Walker, A. R.; Garcia-Varela, A. (20 June 2013). "Variable Stars from the OGLE-III Shallow Survey in the Large Magellanic Cloud". Acta Astronomica. 63 (2): 159–179. arXiv:1306.4802. Bibcode:2013AcA....63..159U.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 3.7 de Wit, S.; Bonanos, A.Z.; Tramper, F.; Yang, M.; Maravelias, G.; Boutsia, K.; Britavskiy, N.; Zapartas, E. (2023). "Properties of luminous red supergiant stars in the Magellanic Clouds". Astronomy and Astrophysics. 669: 17. arXiv:2209.11239. Bibcode:2023A&A...669A..86D. doi:10.1051/0004-6361/202243394. Unknown parameter
|s2cid=ignored (help) - ↑ 4.0 4.1 4.2 4.3 4.4 4.5 4.6 Kamath, D.; Wood, P. R.; Van Winckel, H. (4 August 2015). "Optically visible post-AGB stars, post-RGB stars and young stellar objects in the Large Magellanic Cloud". The Royal Astronomical Society. 454 (2): 1468–1502. arXiv:1508.00670. Bibcode:2015MNRAS.454.1468K. doi:10.1093/mnras/stv1202.
- ↑ 5.0 5.1 Brown, 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. Unknown parameter
|s2cid=ignored (help) Gaia EDR3 record for this source at VizieR. - ↑ Vallenari, A.; et al. (Gaia Collaboration) (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. arXiv:2208.00211. doi:10.1051/0004-6361/202243940. Gaia DR3 record for this source at VizieR.
- ↑ Pietrzyński, G.; Graczyk, D.; Gallenne, A.; Gieren, W.; Thompson, I. B.; Pilecki, B.; Karczmarek, P.; Górski, M.; Suchomska, K.; Taormina, M.; Zgirski, B.; Wielgórski, P.; Kołaczkowski, Z.; Konorski, P.; Villanova, S.; Nardetto, N.; Kervella, P.; Bresolin, F.; Kudritzki, R. P.; Storm, J.; Smolec, R.; Narloch, W. (2019). "A distance to the Large Magellanic Cloud that is precise to one per cent". Nature. 567 (7747): 200–203. arXiv:1903.08096. Bibcode:2019Natur.567..200P. doi:10.1038/s41586-019-0999-4. PMID 30867610. Unknown parameter
|s2cid=ignored (help) - ↑ Ren, Yi; Jiang, Bi-Wei (2020-07-20). "On the Granulation and Irregular Variation of Red Supergiants". The Astrophysical Journal. 898 (1): 24. arXiv:2006.06605. Bibcode:2020ApJ...898...24R. doi:10.3847/1538-4357/ab9c17. ISSN 1538-4357.
- ↑ Henize, Karl G. (1956-05-05). "Catalogues of Hα-emission Stars and Nebulae in the Magellanic Clouds". Astrophysical Journal. 2: 315. Bibcode:1956ApJS....2..315H. doi:10.1086/190025.
- ↑ Westerlund, B. E.; Olander, N.; Hedin, B. (1981). "Supergiant and giant M type stars in the Large Magellanic Cloud". Astronomy & Astrophysics Supplement Series. 43: 267–295. Bibcode:1981A&AS...43..267W.
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