A non-local thermodynamic equilibrium, line-blanketed synthetic spectrum of IOTA Herculis - C, Al, and Si lines

Details A non-local thermodynamic equilibrium, line-blanketed synthetic spectrum of IOTA Herculis - C, Al, and Si lines A non-local thermodynamic equilibrium, line-blanketed synthetic spectrum of IOTA Herculis - C, Al, and Si lines

Oct 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...380..606g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 380, Oct. 20, 1991, p. 606-616. Research supported by National Research Cou

Astronomy and Astrophysics

Astrophysics

8

B Stars, Early Stars, Main Sequence Stars, Stellar Atmospheres, Stellar Spectra, Thermodynamic Equilibrium, Abundance, Aluminum, Carbon, Resonance Lines, Silicon, Stellar Models

Scientific paper

A non-LTE line-blanketed model stellar atmosphere is used to compute a model of I Herculis (B3 IV) with a Teff of 17,500 K and a log g of 3.75, following the conclusions of Peters and Polidan (1985). Detailed profiles of a number of lines of C, Al, and Si in the 1200-2000-A region are computed, including the resonance lines of C II, Al II, and Al III. These profiles are compared to observations obtained from the coaddition of eight IUE SWP images, using a technique developed by Leckrone and Adelman (1989). Comparison of carbon lines with a model that is underabundant in carbon by a factor of 2 relative to the sun indicates that the C abundance of Iota Her is at most one-half solar. Non-LTE effects are examined by comparing an LTE model possessing identical atmospheric parameters with the non-LTE model. Substantial differences in the populations of the model atomic states are found, but differences in the temperature structure of the two models often mask the non-LTE effects in the synthetic spectra.

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