Mass transport mechanism to galactic nuclei in spiral galaxies: effect of supernova explosions

Naomichi Yutani  (Kagoshima University)

Understanding the mechanisms of mass transport to the central nuclei of galaxies is crucial for SMBH formation and, consequently, galaxy formation. However, the mechanisms of mass transport from the host galaxy to the central nucleus within 10 pc remain unclear. In this study, we conducted galaxy formation simulations with N-body/SPH methods considering star formation activity in a high density region (nH >= 10^3 /cc) and AGN feedback to elucidate the mass transport mechanism from 10 kpc scale to the central nucleus within 10 pc. Additionally, using particle splitting methods, we simulated the star formation activity in several kpc of galaxies at high resolution (mass resolution: 600 Msun) and evaluated the relationship between star formation activity and angular momentum transport.  As a result, we find that the dominant angular momentum transport mechanism varies with the strength of the bulge potential within a few hundred pc of the galactic center. In the poster, we also discuss the included gas mass (star formation) in the central nucleus and the angular momentum transport due to spiral arm structures.