分子云中的湍流  

Turbulence in molecular clouds

作　　者：钱磊[1,2] 李菂 潘之辰 

机构地区：[1]中国科学院国家天文台,北京100012 [2]中国科学院射电天文重点实验室,南京210008

出　　处：《中国科学：物理学、力学、天文学》2017年第5期55-60,共6页Scientia Sinica Physica,Mechanica & Astronomica

基　　金：国家重点基础研究发展计划(编号:2012CB821800;2015CB857100)资助项目

摘　　要：湍流是分子云中的重要现象,在恒星形成中发挥了关键作用.湍流研究包括能量注入、能量耗散和间歇性等.湍流能量注入可能来源于星系盘的剪切、引力塌缩以及恒星演化过程的反馈.能量注入机制可能不是唯一的.本文虽尚未明确测量到湍流能量耗散尺度,但可以通过观测确定湍流耗散速率.实测中已经观察到了分子云中湍流的间歇性.未来分子云中的湍流研究还需要大天区、高空间分辨率的谱线成图数据(例如,110m望远镜C_2H谱线、^(13)CO谱线成图)以更好地研究能量注入尺度、注入率、能量耗散率、间歇性以及各向异性等课题.As a fundamental process in molecular clouds, turbulence plays a crucial role in star formation. Important aspects of astro- physical turbulence in molecular clouds include energy injection, energy dissipation, and intermittency. Energy injection for turbulence may come from the shear of galactic disks, gravitational collapse, the feedback of stellar processes, and/or a combination of these processes. Although the dissipation scale is still to be measured with certainty, the turbulence dissi- pation rate can be determined from observation. Intermittency of turbulence has been observed in molecular clouds. Large area spectral line mapping of high spatial resolution （e.g., C2H and 13CO spectral line mapping with QTT） will improve our understanding of energy injection scale and injection rate, energy dissipation rate, intermittency, and anisotropy of turbulence in molecular clouds.

关 键 词：分子云 湍流 

分 类 号：P152[天文地球—天文学]