New method for fast and easy computation of radiative accelerations in stars

Details New method for fast and easy computation of radiative accelerations in stars New method for fast and easy computation of radiative accelerations in stars

Aug 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004mnras.352.1329l&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 352, Issue 4, pp. 1329-1334.

Astronomy and Astrophysics

Astronomy

9

Diffusion, Stars: Abundances, Stars: Chemically Peculiar

Scientific paper

Accurate determination of radiative accelerations of the elements is critical when studying atomic diffusion in stars. However, the computing time necessary to calculate these accelerations can become prohibitive because large atomic and opacity data bases are required. Parametric equations of radiative accelerations due to both bound-bound and bound-free transitions, valid at large optical depths, are presented for the following trace elements: C, N, O, Ne, Na, Mg, Al, Si, S, Ar, Ca and Fe. These equations can easily be implemented in existing astrophysical applications without requiring large computing resources.

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