Chemical abundances of LMC fast-rotators b stars

Details Chemical abundances of LMC fast-rotators b stars Chemical abundances of LMC fast-rotators b stars

Aug 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003basbr..23..123n&link_type=abstract

Boletim da Sociedade Astronômica Brasileira (ISSN 0101-3440), vol.23, no.1, p. 123-123

Astronomy and Astrophysics

Astronomy

Scientific paper

We present chemical abundances for B main sequence fast-rotator stars of the cluster NGC 2004 in the Large Magellanic Cloud (LMC). The spectra were obtained using UVES (ll 3750-5000) on the VLT (ESO) with a resolution of R = 20000 and signal to noise S/N = 50. We use a purely spectroscopic analysis to determine effective temperature, surface gravity, microturbulence of the stars and abundances of a variety of elements (He,C, N, O, Mg, Si, Al). We compare these results with those using photometric determination of Teff. Kurucz ATLAS9 LTE model atmospheres and DETAIL/SURFACE non-LTE line formation are used through the analysis. The targets are unevolved main sequence stars and their abundances reflect those of the progenitor interstellar medium and provide information on stellar and galactic evolution in the LMC. In particular, the elements C, N and O, well observed in the spectra of the stars, potentially constrain scenarios of main sequence rotational mixing. We discuss underabundances of some elements in the Large Magellanic Clouds in comparison with the Galactic thin disk and effects of rotational mixing. Our preliminary results for the star D15 indicate mean differencies of ~ 0.4 dex for derived abundances adopting Teff determined spectroscopically and photometrically. We considered microturbulent velocities using both pure spectroscopic analysis and OII lines. We found a difference of ~ 7 km/s for microturbulent velocity, and ~ 0.2 dex for abundances when adopting the same Teff.

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