SPP 471: Physik der Sternentstehung

在“星星形成物理学”优先方案中，天文学家、天体物理学家、天体化学家和进行数值计算的科学家共同努力，以查明恒星和星团是如何从冷的星际分子云中形成的。原恒星深深嵌入尘埃分子核心，年轻恒星则与星周尘埃盘和扩展的包层有关。因此，红外和亚毫米波连续谱和谱线观测对于我们理解星星的形成起着关键作用。这一过程的特点是温度和密度梯度大，涉及湍流、磁场、旋转、坍缩和外流过程以及不同尺度的辐射传输。大规模数值计算是该计划的重要组成部分。此外，加热和冷却等微物理过程以及化学过程对星星的形成也至关重要。这一主题的复杂性要求具有非常不同科学背景的团体进行合作。

In the priority programme "Physics of Star Formation", astronomers, astrophysicists, astrochemists and scientists performing numerical computations work together in order to find out how stars and stellar clusters form from cool interstellar molecular clouds. Protostars are deeply embedded in dusty molecular cores and young stars are associated with circumstellar dust disks and extended envelopes. Therefore, infrared and submillimeter continuum and line observations play a key role for our understanding of star formation. This process is characterised by large temperature and density gradients and involves turbulence, magnetic fields, rotation, collapse and outflow process as well as radiation transfer on different scales. Large-scale numerical computations form an important part of the programme. In addition, microphysical processes such as heating and cooling and chemical processes are of key importance to star formation. The complexity of the topic requires the collaboration of groups with very different scientific background.