STELLAR EVOLUTION WITH MASS-LOSS - COMPARISON OF NUMERICAL AND SEMIANALYTICAL COMPUTATIONS

We present here results of stellar evolution calculations that include the latest advances in radiative opacities and neutrino cooling, and discuss on the basis of these models how the internal stellar structure responds to mass loss from the stellar surface. This problem has particular importance for the development of semi-analytical algorithms for efficient calculation of synthetic stellar populations with realistic (and hence complex) mass-loss scenarios, We therefore compare our numerical results with test calculations based on a semi-analytical stellar evolution method developed by us. Although small, but important, differences between results from the two methods are revealed, the evolutionary tracks in the Hertzsprung-Russell diagram predicted by the two approaches are almost identical.