摘要
本文给出一批M巨星、s星和碳星的JHKL′宽波段测光及2.3—4μm近红外分光观测结果.结合IRAS观测资料可以发现,M巨星和碳星的1一100μm宽波段测光红外谱形有较为明显的差异,而s星的谱形则基本上介于两者之间.近红外分光结果表明,除了碳星均存在由HCN和C_2H_2导致的处于3.1μm的强吸收外,S星中也有一些存在较弱的上述吸收,而M巨星则没有.以上观测结果可能为晚型星中存在M-S-C的演化序列提供进一步的观测依据.
The JHKL' photometry and 2.3—4μm spectrophotometry of some M giants, S type stars and carbon stars are presented in this paper. It is found that combined with IRAS data, the energy spectra in 1—100μm for S type stars is between those for M giants and carbon stars, which are obviously different. It is found from the spectrophotometry in the near infrared that besides strong absorption at 3.1μm for carbon stars caused by HCN and C_2H_2, weak absorption for some S type stars has been found in the same region. However, no any trace of absorption at 3.1μm for M giants can be seen. It is preliminarily concluded that the above results provide more evidence for the M-S-C sequence in the late stage of stellar evolution.
出处
《天文学报》
CSCD
北大核心
1992年第2期139-145,共7页
Acta Astronomica Sinica
关键词
晚期演化
能谱
恒星
红外观测
Infrared Observation of Late Type Stars—3.1μm Absorption—Late Stage of Stellar Evolution
