The feedback from massive young stars has a profound impact on the interstellar medium (ISM), driving turbulence and regulating star formation. Among many feedback processes, supernovae provide predominant amount of momentum to the ISM in scales larger than individual star forming regions. In this talk, I will review our recent hydrodynamic numerical simulations in local galactic disks, including momentum feedback from supernovae. Our models demonstrate that the star formation rates are regulated to establish all thermal, turbulent, and vertical dynamical equilibria. In addition, synthetic HI 21cm emission and absorption lines constructed from our simulations successfully reproduce and explain the observed distribution of the brightness temperature, optical depth, and spin temperature. Finally, I will introduce our current attempt to quantify a necessary condition for the correct treatment of supernova feedback.