Model atmospheres for G, F, A, B, and O stars

A grid of LTE model atmospheres is presented for effective temperatures ranging from 5500 to 50,000 K, for gravities from the main sequence down to the radiation pressure limit, for abundances solar, 1/10 solar, and 1/100 solar. The models were computed by use of a statistical distribution-function representation of the opacity of almost 10/sup 6/ atomic lines. For each model we tabulate the temperature structure, fluxes, UBV and uvby colors, bolometric correction, and Balmer line profiles. The solar abundance models are compared to narrow, intermediate (by Relyea and Kuruez), and wide (by Relyea and Kuruez and by Buser and Kuruez) band photometry and are found to be in good agreement with the observations for effective temperatures aboue 8000 K. Excellent agreement exists with the spectrophotometry and Balmer line profiles of Vega. A small systematic error in the colors of late A and F stars is probably due to an overestimate of convection in weakly convective models. This error does not seem to affect greatly the use of the predicted colors for differential studies. The solar model has approximately a 2% error in the V flux because molecular lines were not included.