摘要
运用 C O 分子谱线及红外天文卫星资料,求出了金牛座、蛇夫座核心2 个恒星形成区的气体运动温度 Tk 和尘埃温度 Td ,验证了尘埃加热分子云的基本条件;着重探讨了用 Td 参量比较年轻星体演化状态的方法,得出蛇夫座核心区恒星比金牛座恒星年轻的初步结论。
Gas kinetic temperature T k and dust temperature T \-d were obtained for the clouds in Ophiuchus and Taurus based on CO observation as well as IRAS data . The requested T \-d> T k for dust collision heating mechanism has been tested. The relationship between T \-d\, T bol and evolutionary stat es has been analyzed. Results show that young stars in Ophiuchus core are younge r than in those of Taurus, and IRAS colour temperature can be used to estimate t he evolutionary states of young stars as a whole.
出处
《北京大学学报(自然科学版)》
CAS
CSCD
北大核心
1999年第5期665-671,共7页
Acta Scientiarum Naturalium Universitatis Pekinensis
基金
国家自然科学基金
中科院射电天文联合实验室资助项目
关键词
星际分子
分子云
金牛座
热性质
蛇夫座
星体
interstellar molecular
infrared radiation
dynamics of interstellar molecular