CO分子转动谱线的天体物理研究方法和近期进展  

Astrophysical methods and recent proceeding on the researches of CO rotation lines

作　　者：陈亚峰 曾琴[1] 毛瑞青[1] 裴春传[1] 

机构地区：[1]中国科学院紫金山天文台,南京210008

出　　处：《天文学进展》2000年第1期67-74,共8页Progress In Astronomy

基　　金：国家自然科学基金!19973017

摘　　要：ＣＯ的射电转动谱线揭示了光学不可见的冷宇宙、银河系最大天体──巨分子云和恒星形成过程中的一个普遍存在的重要的相──双极外流．ＣＯ在６７～１８６μｍ波段的转动谱线是探测动能温度数百度以上的热天体（诸如富碳、富氧演化星包层，行星状星云、年轻星和恒星形成区复合体）物理条件的重要探针。对ＣＯ分子转动谱线的天体物理研究方法和在该领域的近期进展作了简单的评述。CO rotation lines at radio wavelengths reveal the cold universe which is undetectable by optical instruments, the giant molecular clouds-the largest objects in the Galaxy and the imported phase of the star forming processes-molecular outflow. CO spectra at the wavelength range of 67～186μm are the important probes for detecting the objects of kinetic temperature of several hundred degree, i.e., the envelope of carbon or oxygen rich star, planetary nebular, young stellar object and star forming complex. The main goal of this paper is giving a review towards astrophysical methods and recent proceeding on the research works which base on observing CO rotational lines.

关 键 词：CO 分子转动普线 天体物理 星际介质 研究方法 

分 类 号：P155[天文地球—天文学] P141.5