Time variation in mas accretion rate on protostars due to merging molecular cloud cores
speaker: Yano Yuta
Abstract:
According to the standard theory of star formation, a star forms from a molecular cloud core. It has also been assumed that the physical state of the core determines the evolution and formation of protostars that occur inside the core once it is formed. However, recent observational and theoretical studies suggest that the physical state of the core may be strongly affected by surrounding influences such as accretion and merging/collisions(e.g., Shimajiri et al. 2019; Takemura et al. 2021). For example, hub filament structures may affect the core as global structures of the molecular clouds. If the accretion rate changes as external gas accretes to the hub’s core, it would also affect protostellar outflow. Thus, toward a full understanding of how stars form under realistic conditions, it is important to understand the effects of the core external environments. In this study, we investigate how the mass accretion rate to a central protostar changes when the stable core merges into the core with a protostar formed in the center from the outside. And we use 3D numerical simulations. The results show that core merging increases the mass accretion rate.