Investigating high-mass star formation through chemical compositions of infrared dark clouds

通过红外暗云的化学成分研究大质量恒星的形成

• 批准号: 21740144
• 负责人: SAKAI Takeshi
• 金额: $ 2.91万
• 依托单位: The University of Tokyo
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for Young Scientists (B)
• 财政年份: 2009
• 资助国家: 日本
• 起止时间: 2009 至 2010
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-21740144/
• 关键词: 電波天文学; 星間物質; 星間分子; 赤外暗黒雲; 大質量星形成; SIS受信機; ミリ波; 分子雲; サブミリ波; Infrared dark cloud; 星形成; 可視撮像

We have investigated the high-mass star formation on the basis of the chemical compositions of infrared dark clouds (IRDCs), which are thought to be in early evolutionary stages of high-mass star formation. For this purpose, we have carried out a survey of molecular lines toward massive clumps associated with infrared dark clouds (IRDCs) by using the Nobeyama Radio Observatory 45 m telescope and the ASTE 10 m telescope. We have found that the SiO and CH_3OH abundances relative to H^<13>CO^+ are enhanced in several IRDC clumps. Since SiO and CH_3OH are known as "shock tracers", this results means that an interaction between outflows and dense gas frequently occurs in early evolutionary stages of high-mass star formation. The data obtained are useful for future high-resolution observations.

红外暗云被认为是高质量星星形成的早期演化阶段，我们利用红外暗云的化学成分研究了高质量星星的形成。为此目的，我们进行了调查的分子线向大规模团块与红外暗云（IRDC）的使用野边山射电天文台45米望远镜和ASTE 10米望远镜。我们发现，在几个IRDC团块中，SiO和CH_3OH相对于H^<13>CO^+的丰度增加。由于SiO和CH_3OH被称为“激波示踪物”，这一结果意味着外流和致密气体之间的相互作用经常发生在高质量星星形成的早期演化阶段。所获得的数据对未来的高分辨率观测很有用。

项目成果

A SURVEY OF MOLECULAR LINES TOWARD MASSIVE CLUMPS IN EARLY EVOLUTIONARY STAGES OF HIGH-MASS STAR FORMATION

• DOI: 10.1088/0004-637x/714/2/1658
• 发表时间: 2010-04
• 期刊: The Astrophysical Journal
• 作者: T. Sakai;N. Sakai;T. Hirota;S. Yamamoto