Disk Galaxy Models Driven by Stochastic Self-Propagating Star Formation

We present a model of chemical and spectrophotometric evolution of disk galaxies based on a stochastic self-propagating star formation scenario. The model incorporates galaxy formation through the process of accretion, chemical and photometric evolution treatment, based on simple stellar populations (SSP), and parameterized gas dynamics inside the model. The model reproduces observational data of the late-type spiral galaxy M 33 reasonably well. Promising test results prove the applicability of the model, and the adequate accuracy for the interpretation of disk galaxy properties.