Unveiling the Dynamics of Dense Cores in Cluster-Forming Clumps: A 3D MHD Simulation Study of Angular Momentum and Magnetic Field Properties
Speaker: Shinichi Kinoshita
Abstract:
Almost all stars within the Milky Way form as members of clusters. Dense cores, the direct progenitor of stars, are formed in the cluster-forming clumps and eventually form star clusters. Therefore, comprehending the effect of the clump environment on core properties is important for understanding star formation and galaxy evolution.
We conducted isothermal MHD simulations with self-gravity to investigate the properties of dense cores in cluster-forming clumps. Two different setups were explored: a single rotating clump and colliding clumps. We focused on determining the extent to which the rotation and magnetic field of the parental clump are inherited by the formed dense cores. Our statistical analysis revealed that the alignment between the angular momentum of dense cores, Lcore, and the rotational axis of the clump is influenced by the strength of turbulence and the simulation setup. In single rotating clumps, we found that Lcore tends not to align with the clump’s rotational axis unless the initial turbulence is weak. In colliding clumps, however, this alignment does not occur, regardless of the initial turbulence strength. Our analysis of colliding clumps also revealed that the magnetic field globally bends along the shock-compressed layer, and the mean magnetic field of dense cores, Bcore aligns with it. Both in single rotating clumps and colliding clumps, we found that the angle between Bcore and Lcore is generally random, regardless of the clump properties.