We have developed an efficient and accurate set of mostly analytic formulae, that describe the evolution of stars in a wide range of mass and metallicity from the zero-age main sequence to the tip of the AGB. These formulae are based on interpolation between full detailed stellar models. A particular advantage of this kind of algorithm, compared

We present an algorithm for rapid evolution of binary stars. This incorporates single star evolution based on simple fitting formulae that cover a wide range in mass and metallicity. Mass loss, Roche mass transfer and common-envelope evolution are followed with the changes applied to both the primary and secondary where applicable. Due to the large

We present two selected photoionization models of the extragalactic H ii region NGC 2363, and compare them with three sets of observational data. We discuss the effect of adopting different input parameters. We show that the metallicity of NGC 2363 has most probably been underestimated, and that a value of Z ~= .25 Z_odot is in good agreement with

Solar eigenmodes frequencies are most often determined using some kind of modelisation of the Fourier spectrum of the data in one or two dimensions. Many statistical refinements have lead to significant improvements in the determination of the frequencies and widths of the spectral lines. Nevertheless, this technique relies strongly on several

In a previous work (Eff-Darwich & Pérez-Hernández 1997), it was presented a new inversion method based on the Regularized Least Squares technique. This new method, called OMD (Optimal Mesh Distribution) finds the optimal mesh and smoothing function by means of a deep analysis of the basis functions of the inversion problem. In the present work, the