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OUTFLOWS AND BUBBLES IN TAURUS: STAR-FORMATION FEEDBACK SUFFICIENT TO MAINTAIN TURBULENCE

  • [设施]:500米口径球面射电望远镜
  • [期刊/会议名称]:ApJS
  • [摘要]:We have identified outflows and bubbles in the Taurus molecular cloud based on the ∼100 deg2 Five College Radio Astronomy Observatory 12CO(1-0) and 13CO(1-0) maps and the Spitzer young stellar object catalogs. In the main 44 deg2 area of Taurus, we found 55 outflows, of which 31 were previously unknown. We also found 37 bubbles in the entire 100 deg2 area of Taurus, none of which had been found previously. The total kinetic energy of the identified outflows is estimated to be ~3.9 ´ 1045 erg, which is 1% of the cloud turbulent energy. The total kinetic energy of the detected bubbles is estimated to be ~9.2 ´ 1046 erg, which is 29% of the turbulent energy of Taurus. The energy injection rate from the outflows is ~1.3 ´ 1033 erg s-1, which is 0.4–2 times the dissipation rate of the cloud turbulence. The energy injection rate from bubbles is ~6.4 ´ 1033 erg s−1, which is 2–10 times the turbulent dissipation rate of the cloud. The gravitational binding energy of the cloud is ~1.5 ´ 1048 erg, that is, 385 and 16 times the energy of outflows and bubbles, respectively. We conclude that neither outflows nor bubbles can provide sufficient energy to balance the overall gravitational binding energy and the turbulent energy of Tauru. However, in the current epoch, stellar feedback is sufficient to maintain the observed turbulence in Taurus.
  • [发表日期]:2015
  • [第一作者]:李会贤
  • [第一作者单位]:中国科学院国家天文台
  • [通讯作者]:李会贤、李菂
  • [通讯作者单位]:中国科学院国家天文台
  • [论文类型]:期刊
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  • [关键词]:ISM: bubbles – ISM: individual objects (Taurus) – ISM: jets and outflows – ISM: kinematics and dynamics – surveys – turbulence
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  • [简介]:FAST项目组李会贤等研究人员使用美国FCRAO望远镜观测的一氧化碳谱线巡天数据,在金牛座分子云约100平方度天区里找到了55个外向流和37个气泡,其中31个外向流是新发现的,所有气泡均为首次发现。该研究得到了迄今为止最大连续天区的动力学结构样本。研究结果发表在国际天文期刊ApJ增刊系列上(ApJS, 2015, 219, 20)。审稿人对文章给予高度评价并指出“该工作对恒星形成研究的意义重大,将成为该领域理论及观测方面的一篇重要参考文献。”(“Scientifically, the paper is extremely useful and should be a key reference work in all future theoretical and observational studies of star formation.”)