MHD simulation of cluster formation in clumps
speaker: Kinoshita Shinichi
Abstract:
It is well known that stars are often born in clusters. Thus, understanding cluster formation is very important to grasp the general picture of star formation and the evolution of the galaxy. In recent studies, the cluster-forming clumps are considered to be the parent objects of clusters (Lada & Lada 2003). Cluster-forming clumps tend to exhibit complex velocity structures with several velocity components. One of the hypotheses to explain these velocity fields is the collisions of clumps (e.g., Higuchi et al. 2010). Clump-Clump Collision is proposed as a possible mechanism for triggering the formation of clusters. On the other hand, some studies show that complex velocity structures can be explained by the infalling motion of a single clump with rotation (e.g., Shimoikura et al. 2016). Some expect that such a dynamical infall is a common phenomenon for cluster-forming clumps. In this way, several hypotheses have been proposed, and the formation and evolution processes of clusters still remain unclear.
In this talk, I will show some results of the MHD simulation of cluster formation. We investigated the cluster formation in a single clump infalling with rotation. We will discuss the dynamical evolution of clumps and the properties of dense cores.