CAJ | 학술논문

分子氢的红外振动发射线是显现年轻星质量外流的重要谱线之一。自Gautier等人1976年在猎户座发现年轻星质量外流的分子氢发射开始，人们在银河系内几乎所有的恒星形成区都发现了这种线发射。研究表明，分子氢发射与年轻星周围的其它活动现象(如分子外流和光学喷流)之间有着非常密切的联系。红外和光学喷流代表了年轻星剧烈活动的两个侧面，是喷流与周围介质相互作用强弱不同的表现，这种作用还拖带周围介质，产生分子外流。光学、红外喷流和分子外流组成了恒星形成区壮观的景象，它们是恒星形成活动的重要标志。随着红外探测技术的飞速发展，对年轻星外流活动现象的观测越来越丰富和详细，使人们对这种现象的本质越来越了解。在20世纪90年代NICMOS等大阵列红外探测器投入使用后，红外成像观测有了长足的进步。目前已在70个左右的区域里发现了H2发射，这一数字还在迅速增加。今后的研究主要可能向两个方向发展。其一是高分辨观测，进一步了解H2发射的结构以及与光学喷流和分子外流之间的关系；其二是巡天观测，了解银河系内的恒星形成区H2发射的大尺度结构和恒星形成的统计分布规律
분자경적홍외진동발사선시현현년경성질량외류적중요보선지일。자Gautier등인1976년재작호좌발현년경성질량외류적분자경발사개시，인문재은하계내궤호소유적항성형성구도발현료저충선발사。연구표명，분자경발사여년경성주위적기타활동현상(여분자외류화광학분류)지간유착비상밀절적련계。홍외화광학분류대표료년경성극렬활동적량개측면，시분류여주위개질상호작용강약불동적표현，저충작용환타대주위개질，산생분자외류。광학、홍외분류화분자외류조성료항성형성구장관적경상，타문시항성형성활동적중요표지。 수착홍외탐측기술적비속발전，대년경성외류활동현상적관측월래월봉부화상세，사인문대저충현상적본질월래월료해。재20세기90년대NICMOS등대진렬홍외탐측기투입사용후，홍외성상관측유료장족적진보。목전이재70개좌우적구역리발현료H2발사，저일수자환재신속증가。금후적연구주요가능향량개방향발전。기일시고분변관측，진일보료해H2발사적결구이급여광학분류화분자외류지간적관계；기이시순천관측，료해은하계내적항성형성구H2발사적대척도결구화항성형성적통계분포규률
The infrared ro-vibrational lines of molecular hydrogen are the most important tracers of mass outflow around young stellar objects (YSOs). Since the first discovery by Gautier et al.in 1976, the molecular hydrogen lines have been detected in almost all star forming regions in the Galaxy over the subsequent decades. Further studies show that H2 line emissions are closely associated with other energetic activities around YSOs such as molecular outflows and optical jets. Infrared and optical jets are two different manifestations of the same jet interaction with ambient media. Such interaction leads to the entrainment of ambient material and subsequently drives molecular outflow. Optical/infrared jets and molecular outflows make up the spectacular scenery in the star forming regions and are the signposts of star forming activities. With the advent of the large array detector such as NICMOS in the 1990's, great progress has been made in near infrared imaging observation. So far about 70 regions have been detected in H2 emission, with the number increasing rapidly. Future development will be in two directions: observation at higher angular resolution should reveal the detailed structure of H2 jets, which will also help to understand the relation between H2 emissions, HH jet, and CO outflows; large scale survey will provide information on the large scale structure and distribution of H2 knots in star forming regions in the Galaxy.