弱氦星

弱氦星是化學性質奇特的恆星，它們的光譜在光譜類型有微弱的氦線^[1]^[2]。它們的氦線顯示是在晚期較低的溫度，比氫線顯示的低^[3]。

弱氦星列表编辑

這是一份不完整的弱氦星清單^[4]^[5]：

^ Landstreet, J. D.; Bohlender, David A. Abundance and Magnetic Field Geometries of Helium-Strong and Helium-Weak Stars. Symposium - International Astronomical Union. 1988, 132: 309–312. ISSN 0074-1809. doi:10.1017/S0074180900035191  （英语）.
^ Preston, George W. The Chemically Peculiar Stars of the Upper Main Sequence. Annual Review of Astronomy and Astrophysics. 1974, 12 (1): 257–277. Bibcode:1974ARA&A..12..257P. doi:10.1146/annurev.aa.12.090174.001353.
^ A Digital Spectral Classification Atlas - R. O. Gray. ned.ipac.caltech.edu. [2019-05-31]. （原始内容存档于2020-08-01）.
^ Jaschek, Mercedes; Jaschek, Carlos; Arnal, Marcelo. Helium-Weak Stars. Publications of the Astronomical Society of the Pacific. October 1969, 81 (482): 651. Bibcode:1969PASP...81..650J. doi:10.1086/128832  .
^ Alonso, M. S.; López-García, Z.; Malaroda, S.; Leone, F. Elemental abundance studies of CP stars. The helium-weak stars HD 19400, HD 34797 and HD 35456*. Astronomy and Astrophysics. April 2003, 402: 331. Bibcode:2003A&A...402..331A. doi:10.1051/0004-6361:20030222  .

这是一篇與恆星相關的小作品。你可以通过编辑或修订扩充其内容。