The Interstellar Gas in Star Forming Regions

恒星形成区域的星际气体

基本信息

批准号：
3947-2007
负责人：
Seaquist, Ernest
金额：
$ 3.06万
依托单位：
University of Toronto
依托单位国家：
加拿大
项目类别：
Discovery Grants Program - Individual
财政年份：
2007
资助国家：
加拿大
起止时间：
2007-01-01 至 2008-12-31
项目状态：
已结题

来源：
https://www.nserc-crsng.gc.ca/ase-oro/Details-Detailles_eng.asp?id=361312
关键词：
Interstellar Gas Star Forming Regions

项目摘要

An understanding of the interplay between massive star formation and the properties of the interstellar gas which control it is crucial to comprehending the evolution of the universe. An element of the research plan is to investigate this interaction by observations of nearby galaxies in the millimetre lines of molecules which are tracers of conditions in the interstellar gas. In addition, theoretical computations are being undertaken to simulate the excitation effects of the shock waves produced by the formation of massive stars on the surrounding medium. In this way, it is intended to separate initial gas conditions from those that are the consequences of star formation, especially in galaxies undergoing bursts of massive star formation. In addition, some new ideas will be tested concerning the collective effects on the interstellar gas of the winds of newly born massive stars in large star clusters which are known to be a primary route of star formation in starburst galaxies. In particular, the nature of the numerous compact sources of radio radiation in such galaxies will be the focus of these ideas, since they are currently thought to be the remnants of supernovae, the explosions which end the life of massive stars. If borne out, these ideas will show that they are instead the collective effects of cluster winds, which in turn may considerably modify our understanding of the impact of massive star formation on the surrounding gas. Finally, we will conduct a molecular line study of the star forming potential of gas at the very centre of our own Galaxy in order to understand how this process occurs despite the inhibiting effects of intense ultravioletradiation and gravitational tidal stresses associated with the central region. Emphasis is being placed on certain molecular tracers which will sample the dissociation and evaporation of molecular gas from potential star forming clumps, and reveal the evaporation of the mantles of interstellar dust grains. The study will have relevance to the formation of galaxies and quasars at an early stage of the universe.

了解大规模恒星形成与星际气体的性质之间的相互作用，这对于理解宇宙的演变至关重要。研究计划的一个要素是通过在分子的毫米线中对星系的近距离观察来研究这种相互作用，这些分子是星际气体中条件的示踪剂。此外，还进行了理论计算，以模拟周围介质上大型恒星形成产生的冲击波的兴奋作用。这样，它旨在将初始气体条件与恒星形成后果的气体条件分开，尤其是在经历大型恒星形成的星系中。此外，将测试一些新的想法，以了解对大型明星群中新出生的大型恒星风的集体影响，这是Starburst星系中恒星形成的主要途径。特别是，这些星系中无线电辐射的众多紧凑型来源的性质将是这些想法的重点，因为它们目前被认为是超新星的残余物，即结束大型恒星生命的爆炸。如果出生的话，这些想法将表明它们是群集风的集体影响，进而可以大大改变我们对巨大恒星形成对周围气体的影响的理解。最后，我们将对我们自己星系中心的气体形成恒星形成潜力的分子线研究，以了解尽管与中央区域相关的强烈的紫外线辐射和重力潮汐应力受到抑制作用。重点放在某些分子示踪剂上，这些示踪剂将对潜在的恒星形成簇的分子气体的解离和蒸发，并揭示星际尘埃晶粒的披风的蒸发。该研究将与宇宙早期的星系和类星体的形成有关。