  We study various implementations of supernova feedback model and present the
results of our `Osaka feedback model' using isolated galaxy simulations
performed by the smoothed particle hydrodynamics (SPH) code {\small GADGET-3}.
Our model is a modified version of Stinson et al.'s work, and we newly add the
momentum kick for SN feedback rather than only thermal feedback. We incorporate
the physical properties of SN remnants from the results of Chevalier and McKee
\& Ostriker, such as the effective radius of SN bubble and the remnant
life-time, in the form of Sedov-Taylor (ST)-like solutions with the effect of
radiative cooling. Our model utilizes the local, physical parameters such as
density and temperature of the ISM rather than galactic or halo properties to
determine the galactic wind velocity or mass-loading factor. The Osaka model
succeeds in self-regulating star formation, and naturally produces galactic
outflow with variable velocities depending on the local environment and
available SN energy as a function of time.An important addition to our previous
work by Aoyama et al. is the implementation of the {\small CELib} chemistry
library which allows us to deal with the time-dependent input of energy and
metal yields for type Ia \& II supernovae (SNe) and asymptotic giant branch
(AGB) stars. As initial tests of our model, we apply it to isolated galaxy
simulations, and examine various galactic properties and compare with
observational data including metal abundances.
