The formation of weak metal lines in the atmosphere of O-stars - The role of microturbulence and transonic matter outflow

Details The formation of weak metal lines in the atmosphere of O-stars - The role of microturbulence and transonic matter outflow The formation of weak metal lines in the atmosphere of O-stars - The role of microturbulence and transonic matter outflow

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...266..395k&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 266, no. 1, p. 395-401.

Statistics

Computation

43

Metallicity, O Stars, Stellar Atmospheres, Stellar Winds, Turbulence Effects, Computational Astrophysics, Line Spectra, Radiative Transfer, Stellar Mass Ejection, Stellar Spectrophotometry

Scientific paper

The influence of velocity fields from radiation driven winds on the formation of weak metal lines in the atmosphere of O-stars is investigated by the use of a simple atmospheric model. It is found that the transonic velocity field has a significant effect on the observable line equivalent widths, in particular for ions of large atomic weights such as iron. Hydrostatic calculations neglecting the velocity field need significantly higher microturbulent velocities to achieve the same equivalent widths. It is shown that effects of transonic matter outflow on the shape of the profiles of weak metal lines are masked by the usual high rotational velocities of O-stars. We conclude that the inclusion of velocity fields in the radiative transfer is extremely important for the determination of metal abundances from the weak 'pseudophotospheric' metal lines in the optical and ultra-violet spectra of O-stars.

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