BAT99-116
| 觀測資料 曆元 J2000.0 | |
|---|---|
| 星座 | 剑鱼座 |
| 星官 | |
| 赤經 | 5h 38m 44.26s[1] |
| 赤緯 | −69° 06′ 05.88″[1] |
| 視星等（V） | 13.09[1] |
| 特性 | |
| 演化阶段 | 沃尔夫-拉叶星 |
| 光谱分类 | WN5h:a[2] |
| B−V 色指数 | +0.25[1] |
| 天体测定 | |
| 距离 | 163,000 ly (49,970[3] pc) |
| 绝对星等 (MV) | -7.9[1] |
| 詳細資料 | |
| 質量 | 179[4] M☉ |
| 半徑 | 20[2] R☉ |
| 亮度 | 7,079,000[5] L☉ |
| 溫度 | 53,000[1] K |
| 年齡 | ~1.7[6] Myr |
| 其他命名 | |
BAT99 116, [HSH95] 8, Melnick 34, 2MASS J05384424-6906058, Brey 84
| |
| 參考資料庫 | |
| SIMBAD | 资料 |
BAT99-116(也被称为Melnick 34或Mk34)是一颗拥有极高质量和光度的沃尔夫-拉叶星，它位于大麦哲伦星系的剑鱼座30复合体(也被称为蜘蛛星云：NGC 2070)内靠近超星团R136的位置。
双星[编辑]
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由于BAT99-116出现只有星风互撞双星才会出现的大量X射线辐射以及光度周期性的变化，BAT99-116被普遍认为是周期为155天的双星系统。[7]
物理特性[编辑]
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BAT99-116是一颗表面温度超过50,000K的沃尔夫-拉叶星。[2][1]据推测，BAT-116在诞生之初约有275 M☉，[5]此类恒星将会产生极强的恒星风，在其诞生以来BAT99-116已经损失了几十倍太阳质量。[4]由于BAT99-116处于双星系统内，其本身更的温度、光度以及质量都是难以确定的。[2]
演化[编辑]
尽管由于内部的对流融合使得BAT99-116的表面出现了氦和氮的发射谱线，但目前仍普遍认为BAT99-116还处于氢燃烧阶段。 据推断，BAT99-116将很快成为氢耗尽的沃尔夫-拉叶星，届时它将成为一颗蓝特超巨星或高光度蓝变星。再之后BAT99-116将不断的脱去其外壳，成为一颗光谱为WO型、表面温度接近200,000K的沃尔夫-拉叶星，最终BAT99-116将会发生Ic型的超新星爆发而成为黑洞。[8]
参考[编辑]
- ^ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 Doran, E. I.; Crowther, P. A.; de Koter, A.; Evans, C. J.; McEvoy, C.; Walborn, N. R.; Bastian, N.; Bestenlehner, J. M.; Grafener, G.; Herrero, A.; Kohler, K.; Maiz Apellaniz, J.; Najarro, F.; Puls, J.; Sana, H.; Schneider, F. R. N.; Taylor, W. D.; van Loon, J. Th.; Vink, J. S. The VLT-FLAMES Tarantula Survey - XI. A census of the hot luminous stars and their feedback in 30 Doradus. Astronomy & Astrophysics. 2013, 558: 134. Bibcode:2013A&A...558A.134D. arXiv:1308.3412
. doi:10.1051/0004-6361/201321824.
- ^ 2.0 2.1 2.2 2.3 Hainich, R.; Rühling, U.; Todt, H.; Oskinova, L. M.; Liermann, A.; Gräfener, G.; Foellmi, C.; Schnurr, O.; Hamann, W. -R. The Wolf-Rayet stars in the Large Magellanic Cloud. Astronomy & Astrophysics. 2014, 565: A27. Bibcode:2014A&A...565A..27H. arXiv:1401.5474 . doi:10.1051/0004-6361/201322696.
- ^ Pietrzyński, G; D. Graczyk; W. Gieren; I. B. Thompson; B. Pilecki; A. Udalski; I. Soszyński; et al. An eclipsing-binary distance to the Large Magellanic Cloud accurate to two per cent. Nature. 7 March 2013, 495 (7439): 76–79. Bibcode:2013Natur.495...76P. PMID 23467166. arXiv:1303.2063 . doi:10.1038/nature11878.
- ^ 4.0 4.1 Portegies Zwart, Simon F.; Pooley, David; Lewin, Walter H. G. A Dozen Colliding-Wind X-Ray Binaries in the Star Cluster R136 in the 30 Doradus Region. The Astrophysical Journal. 2002, 574 (2): 762. Bibcode:2002ApJ...574..762P. arXiv:astro-ph/0106109 . doi:10.1086/340996.
- ^ 5.0 5.1 Crowther, Paul A.; Caballero-Nieves, S. M.; Bostroem, K. A.; Maíz Apellániz, J.; Schneider, F. R. N.; Walborn, N. R.; Angus, C. R.; Brott, I.; Bonanos, A.; De Koter, A.; De Mink, S. E.; Evans, C. J.; Gräfener, G.; Herrero, A.; Howarth, I. D.; Langer, N.; Lennon, D. J.; Puls, J.; Sana, H.; Vink, J. S. The R136 star cluster dissected with Hubble Space Telescope/STIS. I. Far-ultraviolet spectroscopic census and the origin of He II λ1640 in young star clusters. Monthly Notices of the Royal Astronomical Society. 2016, 458: 624. Bibcode:2016MNRAS.458..624C. arXiv:1603.04994 . doi:10.1093/mnras/stw273.
- ^ Crowther, P. A.; Schnurr, O.; Hirschi, R.; Yusof, N.; Parker, R. J.; Goodwin, S. P.; Kassim, H. A. The R136 star cluster hosts several stars whose individual masses greatly exceed the accepted 150 M⊙ stellar mass limit. Monthly Notices of the Royal Astronomical Society. 2010, 408 (2): 731. Bibcode:2010MNRAS.408..731C. arXiv:1007.3284 . doi:10.1111/j.1365-2966.2010.17167.x.
- ^ Pollock, A. M. T; Crowther, P. A; Tehrani, K; Broos, Patrick S; Townsley, Leisa K. The 155-day X-ray cycle of the very massive Wolf-Rayet star Melnick 34 in the Large Magellanic Cloud. Monthly Notices of the Royal Astronomical Society. 2017. Bibcode:2018MNRAS.474.3228P. doi:10.1093/mnras/stx2879.
- ^ Groh, J. H.; Meynet, G.; Georgy, C.; Ekström, S. Fundamental properties of core-collapse supernova and GRB progenitors: Predicting the look of massive stars before death. Astronomy & Astrophysics. 2013, 558: A131. Bibcode:2013A&A...558A.131G. arXiv:1308.4681 . doi:10.1051/0004-6361/201321906.
