Osaka Feedback Model II: Modeling Supernova Feedback Based on
  High-Resolution Simulations
  Feedback from supernovae (SNe) is an essential mechanism that self-regulates
the growth of galaxies, and a better model of SN feedback is still needed in
galaxy formation simulations. In the first part of this paper, using an
Eulerian hydrodynamic code Athena++, we find universal scaling relations for
the time evolution of momentum and radius for a superbubble, when the momentum
and time are scaled by those at the shell-formation time. In the second part of
this paper, we develop an SN feedback model based on the Athena++ simulation
results utilizing Voronoi tesselation around each star particle, and implement
it into the GADGET3-Osaka smoothed particle hydrodynamic code. Our feedback
model was demonstrated to be isotropic and conservative in terms of energy and
momentum. We examined the mass/energy/metal loading factors and find that our
stochastic thermal feedback model produced galactic outflow that carries metals
high above the galactic plane but with weak suppression of star formation.
Additional mechanical feedback further suppressed star formation and brought
the simulation results in better agreement with the observations of the
Kennicutt--Schmidt relation, with all the results being within the
uncertainties of observed data. We argue that both thermal and mechanical
feedback are necessary for the SN feedback model of galaxy evolution when an
individual SN bubble is unresolved.
