BAT99-116
觀測資料 曆元 J2000.0 | |
---|---|
星座 | 劍魚座 |
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 | |
演化階段 | 沃爾夫-拉葉星 |
光譜分類 | WN5h:a[2] |
B−V 色指數 | +0.25[1] |
天體測定 | |
距離 | 163,000 ly (49,970[3] pc) |
絕對星等 (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 | 資料 |
BAT99-116(也被稱為Melnick 34或Mk34)是一顆擁有極高質量和光度的沃爾夫-拉葉星,它位於大麥哲倫星系的劍魚座30複合體(也被稱為蜘蛛星雲:NGC 2070)內靠近超星團R136的位置。
雙星
![](http://images.weserv.nl/?url=//upload.wikimedia.org/wikipedia/commons/thumb/c/c1/ESO_-_Eso1030a_%28by%29.jpg/220px-ESO_-_Eso1030a_%28by%29.jpg)
由於BAT99-116出現只有星風互撞雙星才會出現的大量X射線輻射以及光度周期性的變化,BAT99-116被普遍認為是周期為155天的雙星系統。[7]
物理特性
![](http://images.weserv.nl/?url=//upload.wikimedia.org/wikipedia/commons/thumb/2/25/Grand_star-forming_region_R136_in_NGC_2070_%28captured_by_the_Hubble_Space_Telescope%29.jpg/220px-Grand_star-forming_region_R136_in_NGC_2070_%28captured_by_the_Hubble_Space_Telescope%29.jpg)
BAT99-116是一顆表面溫度超過50,000K的沃爾夫-拉葉星。[2][1]據推測,BAT-116在誕生之初約有275 M☉,[5]此類恆星將會產生極強的恆星風,在其誕生以來BAT99-116已經損失了幾十倍太陽質量。[4]由於BAT99-116處於雙星系統內,其本身更的溫度、光度以及質量都是難以確定的。[2]
演化
儘管由於內部的對流融合使得BAT99-116的表面出現了氦和氮的發射譜線,但目前仍普遍認為BAT99-116還處於氫燃燒階段。 據推斷,BAT99-116將很快成為氫耗盡的沃爾夫-拉葉星,屆時它將成為一顆藍特超巨星或高光度藍變星。再之後BAT99-116將不斷的脫去其外殼,成為一顆光譜為WO型、表面溫度接近200,000K的沃爾夫-拉葉星,最終BAT99-116將會發生Ic型的超新星爆發而成為黑洞。[8]
參考
- ^ 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.
外部連結