Abstract
Radiative accelerations are quantities that are crucial in the study of diffusion processes in stars. Their calculation requires the use of large atomic and opacity data bases, and generally necessitates very heavy numerical computations. New approximate formulae for radiative accelerations in stars, arising from both bound-bound and bound-free transitions, are presented. These are written in a parametric form, which separate the terms depending on the local abundance of the element under consideration from those depending mainly on the atomic data. These formulae are shown to be significantly superior to those previously published. The main reason for this improvement comes form the use of monochromatic opacities instead of approximating these by the Rosseland mean. The principal advantage for the use of these parametric equations over other methods for calculating radiative accelerations is its numerical expediency. Results are shown for several elements (C, Ar, Ca and Fe) in a type A star.
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