[en] The behavior of pulsation in the outer layers of a ''typical'' Mira variable (M=M/sub sun/,L=10⁴L/sub sun/, T/sub eff/=2750 K,P=373 days) has been studied in the adiabatic and isothermal limits. A shock wave propagates outward once per period, and the radial velocity obtained from observations of hydrogen emission lines is identified with the velocity of gas in the postshock region. In the adiabatic case, mass loss in the form of a steady stellar wind was produced. However, the behavior of the postshock velocity does not agree well with observations, and the mass loss rate is far too large (0.02M/sub sun/yr^-1) if approximate observational estimates of the photospheric density are adopted. In the isothermal case, no continuous mass loss was produced but occasional ejection of shells occurs. The time-averaged mass loss rate produced by this process is approx.10^-12M/sub sun/yr^-1. The time-dependence and magnitude of the emission line velocity is in reasonable agreement with observations. In a strongly driven model, a type of behavior was found which may explain the alternating high and low minima observed in RV Tauri variable and some Miras (e.g.,R Cen). Pulsation introduced into a star undergoing steady mass loss as a result of radiation pressure acting on grains caused the mass loss rate to increase by a factor of approx.40 while the terminal velocity of the flow was almost unaltered