WR 25
| 观测资料 历元 J2000.0 | |
|---|---|
| 星座 | 船底座 |
| 星官 | |
| 赤经 | 10h 44m 10.337s[1] |
| 赤纬 | -59° 43′ 11.41″[1] |
| 视星等（V） | 8.80[2] |
| 特性 | |
| 演化阶段 | 沃夫–瑞叶星 |
| 光谱分类 | O2.5If*/WN6 + OB[3] |
| 天体测定 | |
| 径向速度 (Rv) | −34.6[4] km/s |
| 自行 (μ) | 赤经：−6.813±0.057[5] mas/yr 赤纬：2.721±0.055[5] mas/yr |
| 视差 (π) | 0.4763 ± 0.0329[5] mas |
| 距离 | 6,800 ± 500 ly (2,100 ± 100 pc) |
| 绝对星等 (MV) | -6.98[6] |
| 轨道[4] | |
| 绕行周期 (P) | 207.85 days |
| 半长轴 (a) | 156 R☉ |
| 偏心率 (e) | 0.50 |
| 半振幅 (K1) (primary) | 44 km/s |
| 详细资料 | |
| WR | |
| 质量 | 98[6] M☉ |
| 半径 | 20.24[6] R☉ |
| 亮度 (bolometric) | 2,400,000[6] L☉ |
| 温度 | 50,100[6] K |
| 其他命名 | |
| 参考数据库 | |
| SIMBAD | 资料 |
WR 25（HD 93162）是在船底座星云湍流恒星形成区的联星系统，距离地球大约6,800光年。它包含一颗沃夫–瑞叶星和一颗热且明亮伴星，并且是川普勒16星团的成员。
光谱
[编辑]WR 25因为它的亮度和光谱以宽发射线为主，在19世纪就被认定为沃夫–瑞叶星[7]。它的光谱包含氢线，介于经典的WN星和O型超巨星之间。这导致早期报告是联星，例如WN7星加上O7的恒星[8]。它也被描述为WN7 + abs[9]和WN6ha[10]。WR 25的光谱被归类为特定分类引进的热斜杠星，O2.5If*/WN6 。由许多微弱的发射谱线，认识到有氮的存在，还有一些氢和氦的吸收线。这个分类表示比WN6ha光谱类型更精细，有更弱的发射线和更强的吸收线[11]。但是无法清楚的检测到伴星的光谱，而对伴星的认识毫无贡献[4]。
性质
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WR 25系统的主星大约比太阳亮240万倍，并照亮了川普勒16星团的远端。用于推导恒星参数的模型不适合在联星系统中使用，作者指出伴星占系统亮度的15%以上，因此亮度极不稳定。早先基于电离通量测量的估计所产生的值为太阳的150万倍，其它物理数据的估计值也相应降低[12]。
伴星被认为是一颗年轻的炙热大质量恒星，类似于其它已知的WR + O 或WR + WR联星。据报导，它曾被视为O4超巨星，但后续的测量仍然不确定确实的光谱类型。两颗炙热恒星的恒星风碰撞，产生硬X射线[13]，而早在检测到208天的轨道周期之前出，就怀疑是联星[4]。
WR 25虽然非常明亮，但由于星云中大量灰尘的消光，以及大部分的辐射是在紫外线，所以无法以肉眼看见，而只能在X射线和红外线中观测[13][14]。
WR 25位于川普勒16星团的西侧边界处，是银河系中最巨大的OB星协船底座OB1的一部分[15]。由于它极端的亮度，对恒星环境有极大的影响，从恒星移动离开的细长弧线和细丝中可以看到手指星云[16]。
相关条目
[编辑]参考资料
[编辑]- ^ 1.0 1.1 Roeser, S.; Bastian, U. A new star catalogue of SAO type. Astronomy and Astrophysics Supplement Series. 1988, 74: 449. Bibcode:1988A&AS...74..449R. ISSN 0365-0138.
- ^ Ducati, J. R. VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system. CDS/ADC Collection of Electronic Catalogues. 2002, 2237: 0. Bibcode:2002yCat.2237....0D.
- ^ Sota, A.; Maíz Apellániz, J.; Morrell, N. I.; Barbá, R. H.; Walborn, N. R.; Gamen, R. C.; Arias, J. I.; Alfaro, E. J. The Galactic O-Star Spectroscopic Survey (GOSSS). II. Bright Southern Stars. The Astrophysical Journal Supplement. 2014, 211 (1): 10. Bibcode:2014ApJS..211...10S. arXiv:1312.6222
. doi:10.1088/0067-0049/211/1/10.
- ^ 4.0 4.1 4.2 4.3 Gamen, R.; Gosset, E.; Morrell, N.; Niemela, V.; Sana, H.; Nazé, Y.; Rauw, G.; Barbá, R.; Solivella, G. The first orbital solution for the massive colliding-wind binary HD 93162 (≡WR 25). Astronomy and Astrophysics. 2006, 460 (3): 777–782. Bibcode:2006A&A...460..777G. arXiv:astro-ph/0609454 . doi:10.1051/0004-6361:20065618.
- ^ 5.0 5.1 5.2 Brown, A. G. A.; Vallenari, A.; Prusti, T.; de Bruijne, J. H. J.; et al. Gaia Data Release 2. Summary of the contents and survey properties. Astronomy & Astrophysics. 2018. Bibcode:2018A&A...616A...1G. arXiv:1804.09365 . doi:10.1051/0004-6361/201833051. VizieR中此天体在盖亚望远镜第二批数据发布的记录
- ^ 6.0 6.1 6.2 6.3 6.4 Sota, A.; Maíz Apellániz, J.; Morrell, N. I.; Barbá, R. H.; Walborn, N. R.; Gamen, R. C.; Arias, J. I.; Alfaro, E. J.; Oskinova, L. M. The Galactic WN stars revisited. Impact of Gaia distances on fundamental stellar parameters. 2019. arXiv:1904.04687 [astro-ph.SR].
- ^ Campbell, W. W. The Wolf-Rayet stars. Astronomy and Astro-Physics. 1894, 13: 448. Bibcode:1894AstAp..13..448C.
- ^ Smith, Lindsey F. A revised spectral classification system and a new catalogue for galactic Wolf-Rayet stars. Monthly Notices of the Royal Astronomical Society. 1968, 138: 109–121. Bibcode:1968MNRAS.138..109S. doi:10.1093/mnras/138.1.109 .
- ^ Crowther, Paul A.; Smith, Linda J.; Hillier, D. John. Tailored analyses of 24 Galactic WN stars. Space Science Reviews. 1993, 66 (1–4): 271–275. Bibcode:1993SSRv...66..271C. doi:10.1007/BF00771076.
- ^ Smith, Lindsey F.; Maeder, A. The relationship between the WR classification and stellar models. II. The WN stars without hydrogen. Astronomy and Astrophysics. 1998, 334: 845. Bibcode:1998A&A...334..845S.
- ^ Crowther, Paul A.; Walborn, Nolan R. Spectral classification of O2-3.5 If*/WN5-7 stars. Monthly Notices of the Royal Astronomical Society. 2011, 416 (2): 1311. Bibcode:2011MNRAS.416.1311C. arXiv:1105.4757 . doi:10.1111/j.1365-2966.2011.19129.x.
- ^ Crowther, P. A.; Dessart, L. Quantitative spectroscopy of Wolf--Rayet stars in HD 97950 and R136a -- the cores of giant H II regions. Monthly Notices of the Royal Astronomical Society. 1998, 296 (3): 622–642. Bibcode:1998MNRAS.296..622C. doi:10.1046/j.1365-8711.1998.01400.x .
- ^ 13.0 13.1 Pandey, J. C.; Pandey, S. B.; Karmakar, S. Phase-Resolvedxmm-Newtonandswiftobservations of Wr 25. The Astrophysical Journal. 2014, 788 (1): 84. Bibcode:2014ApJ...788...84P. arXiv:1405.7137 . doi:10.1088/0004-637X/788/1/84.
- ^ Sanchawala, K.; Chen, W. P.; Lee, H. T.; Chu, Y. H.; Nakajima, Y.; Tamura, M.; Baba, D.; Sato, S. An X‐Ray and Near‐Infrared Study of Young Stars in the Carina Nebula. The Astrophysical Journal. 2007, 656 (1): 462–473. Bibcode:2007ApJ...656..462S. CiteSeerX 10.1.1.667.3955 . doi:10.1086/510184.
- ^ Wolk, Scott J.; Broos, Patrick S.; Getman, Konstantin V.; Feigelson, Eric D.; Preibisch, Thomas; Townsley, Leisa K.; Wang, Junfeng; Stassun, Keivan G.; King, Robert R.; McCaughrean, Mark J.; Moffat, Anthony F. J.; Zinnecker, Hans. The Chandra Carina Complex Project View of Trumpler 16. The Astrophysical Journal Supplement. 2011, 194 (1): 12. Bibcode:2011ApJS..194...12W. arXiv:1103.1126 . doi:10.1088/0067-0049/194/1/12.
- ^ Walborn, Nolan R. The Company Eta Carinae Keeps: Stellar and Interstellar Content of the Carina Nebula. Eta Carinae and the Supernova Impostors. Astrophysics and Space Science Library. 2012, 384: 25–42. Bibcode:2012ASSL..384...25W. ISBN 978-1-4614-2274-7. doi:10.1007/978-1-4614-2275-4_2.
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