Determination of Chemical Abundances in Fast Rotating Stars

Details Determination of Chemical Abundances in Fast Rotating Stars Determination of Chemical Abundances in Fast Rotating Stars

Jun 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002sf2a.conf..525f&link_type=abstract

SF2A-2002: Semaine de l'Astrophysique Francaise, meeting held in Paris, France, June 24-29, 2002, Eds.: F. Combes and D. Barret,

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

Late O, B and early A type stars, dwarfs to giants which have shown at least once emission in the hydrogen line series are called Be stars. The common characteristics of these objects is the high rotation which on average is at 80% of the critical one. As these stars are near or likely in the main sequence, they can be considered being still in a stable evolutionary stage and their surface chemical abundance should, in principle, mirror the chemical composition of the protostellar environment. Theoretical models of the evolution of rotating stars predict, however, some contamination of the atmosphere by yields owing to the CNO cycle in the stellar core, favored by a turbulent diffusion of elements. The abundance analysis of CNO elements done so far on ``normal" OB stars show some N enrichment and no change for C. These stars are however low rotators, where the meridional circulation is rather long ranging from 1e6 to 1e8 yr. This kind of time scale is however smaller by a factor 1e2 in Be stars, so that the expected mixing should, if exists, take place. We present in this contribution the results obtained on the abundance determination of a small number of Be stars with Vsin(i) < 150 km s of CNO elements and He. We use for that hemisphere-recomposed non-LTE models of stellar atmospheres for highly rotating stars.

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