Stellar evolution with mass loss { comparison of numerical and semi - analytical computations

Abstract

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 e cient 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, di erences between results from the two methods are revealed, the evolutionary tracks in the HR-diagram predicted by the two approaches are almost identical.

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Cite this paper

@inproceedings{Jimenez1995StellarEW, title={Stellar evolution with mass loss \{ comparison of numerical and semi - analytical computations}, author={Raul Jimenez and Peter Thejll and James Macdonald}, year={1995} }