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The ``galactic shocks'' \citep{fujimoto68,roberts69} is investigated using afull three-dimensional hydrodynamic simulations, taking into accountself-gravity of the ISM, radiative cooling, and star formation followed byenergy feedback from supernovae. This is an essential progress from theprevious numerical models, in which 2-D isothermal, non-self-gravitating gas isassumed. We find that the classic galactic shocks appears is unstable andtransient, and it shifts to a globally quasi-steady, inhomogeneous pattern dueto non-linear development of instabilities in the disk. The spiral patternsconsists of many GMC-like dense condensations, but those local structures arenot steady, and they evolves into irregular spurs in the inter-arm regions.Energy feedback from supernovae do not destroy the quasi-steady spiral arms,but it mainly contributes to vertical motion and structures of the ISM.

Instabilities of Spiral Shocks -- II. A quasi-steady State in the multi-phase inhomogeneous ISM