  We examine the properties of spiral shocks from a steady, adiabatic,
non-axisymmetric accretion disk around a compact star in binary. We first time
incorporate all the possible influences from binary through adopting the Roche
potential and Coriolis forces in the basic conservation equations. In this
paper, we assume the spiral shocks to be point-wise self-similar, and the flow
is in vertical hydrostatic equilibrium to simplify the study. We also
investigate the mass outflow due to the shock compression and apply it to the
accreting white dwarf in binary. We find that our model will be beneficial to
overcome the ad hoc assumption of optically thick wind generally used in the
studies of the progenitor of supernovae Ia.
