麦哲伦桥
| 分类 | 星系传输中性氢区 |
|---|---|
| 赤经 | 03h 11m |
| 赤纬 | -77.5° |
 维基共享资源相关媒体 | |
[编辑维基数据] | |
麦哲伦桥（Magellanic Bridge）是连接大小麦哲伦云的一条由中性氢组成的气流[1]。它的特征是气体的金属量很低，并且仅曾在其中发现少量的恒星[2][3]。不要将它与麦哲伦星流混淆在一起，后者将麦哲伦云与银河系连结在一起，是J. V. Hindman等人在1963年发现的[4]。
参考资料
- ^ Putman, M. E. The Magellanic System's Interactive Formations. Publications of the Astronomical Society of Australia. 2000, 17 (1). Bibcode:2000PASA...17....1P. ISSN 1323-3580. doi:10.1071/AS00001 （英语）.
- ^ Lehner, N. FUSE Observations of the Magellanic Bridge. American Astronomical Society Meeting Abstracts. 2001-12, 199: 65.06 [2020-07-14]. （原始内容存档于2020-03-13） （英语）.
- ^ Lehner, N. Far‐Ultraviolet Spectroscopic Explorer Observations of the Magellanic Bridge Gas toward Two Early‐Type Stars: Molecules, Physical Conditions, and Relative Abundances. The Astrophysical Journal. 2002-10-10, 578 (1) [2022-11-23]. Bibcode:2002ApJ...578..126L. ISSN 0004-637X. arXiv:astro-ph/0206250
. doi:10.1086/342349. （原始内容存档于2022-11-23） （英语）.
- ^ Harris, Jason. The Magellanic Bridge: The Nearest Purely Tidal Stellar Population. The Astrophysical Journal. 2007-03-20, 658 (1): 345 [2020-07-14]. ISSN 0004-637X. doi:10.1086/511816. （原始内容存档于2020-07-14） （英语）.
- SIMBAD, "Magellanic Bridge"（页面存档备份，存于互联网档案馆） (accessed 12 April 2010)
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