Welcome on the help webpages for the calculation of radiative accelerations in stars

Evaluation of radiative accelerations is important for computing element segregation in stars. Radiative acceleration is often the leading component in atomic diffusion process, which causes inhomogeneous abundance distribution of elements. This physical process is efficient when mixing processes (turbulence, convection, large scale circulations, etc...) are weak enough. This is especially the case in stellar radiative zones, where turbulence and convection do not take place.

Calculation of accurate radiative acceleration for a given chemical element often requires large computing ressources. In particular, it needs the numerical integration over frequency of the local monochromatic radiation flux weighted by cross-sections of photoabsorption for all atomic transitions of all ions existing in the considered medium. There are several methods to carry out this computation, from explicit evaluations (detailed and accurate) to semi-analytic (or parametric) approximations. On this website, some downloadable data for the numerically efficient semi-analytic method called SVP approximation are provided (Alecian & LeBlanc 2002, see also Alecian & Artru 1990, LeBlanc & Alecian 2004). The SVP approximation is only valid in optically thick layers (stellar interiors) and for stars with masses larger than 1 solar mass.


Update: February 2019

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