Model atmosphere including microscopic diffusion

Details Model atmosphere including microscopic diffusion Model atmosphere including microscopic diffusion

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001sf2a.conf..185h&link_type=abstract

Abstracts from SF2A-2001: Semaine de l'Astrophysique Francaise, meeting held in Lyon, France, May 28-June 1st, 2001, Eds.: F. Co

Astronomy and Astrophysics

Astrophysics

Scientific paper

Certain stars present abundances very different from those expected (Chemically Peculiar stars). It is supposed that this behavior is due to microscopic diffusion of the chemical elements. This process generates a stratification of the abundances, different for each element, leading to an enrichment or a depletion in the line forming zone. In hot stars, diffusion occurs in the atmosphere, and the main difficulty is the need to solve explicitly the radiative transfer equation. I will present a modern code of calculation of diffusion, developed from the model atmosphere code Phoenix, and the results obtained.

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