  We have developed a self-consistent physical model for super stellar cluster
winds based on combining a 1-D steady-state adiabatic wind solution and a
non-equilibrium ionization calculation. Comparing with the case of collisional
ionization equilibrium, we find that the non-equilibrium ionization effect is
significant in the regime of a high ratio of energy to mass input rate and
manifests in a stronger soft X-ray flux in the inner region of the star
cluster. Implementing the model in X-ray data analysis softwares (e.g., XSPEC)
directly facilitates comparisons with X-ray observations. Physical quantities
such as the mass and energy input rates of stellar winds can be estimated by
fitting observed X-ray spectra. The fitted parameters may then be compared with
independent measurements from other wavelengths. Applying our model to the star
cluster NGC 3603, we find that the wind accounts for no more than 50% of the
total "diffuse" emission, and the derived mass input rate and terminal velocity
are comparable to other empirical estimates. The remaining emission most likely
originate from numerous low-mass pre-main-sequence stellar objects.
