ABUNDANCE ANALYSIS OF ROAP STARS .2. HD-203932

A new tool to simplify abundance analyses which is based on stand-alon e programs has been applied to the rapidly oscillating Ap star HD 2039 32 (BI Mic, CD -30 degrees 18600, SAO 212996; Ap(SrEu), V = 8.82 mag). The spectroscopically determined T-eff = 7450+/-100 K and log g = 43/-0.15 put this star close to the ZAMS. Other fundamental atmospheric parameters are v(micro) < 0.6 km s(-1) and the total abundance of all iron peak elements [M/H] = 0.0+/-0.1. The fundamental parameters put H D 203932 in a region of the HR-diagram where convection starts becomin g efficient and the standard mixing length theory models lead to sever e problems in the determination of the atmospheric parameters. The dif ference between the upper limit for log g obtained from several varian ts of the mixing length theory and the Canuto-Mazzitelli model indicat es that the choice of a particular convection model can influence the determination of basic stellar parameters. For the first time abundanc es were determined for HD 203932 showing a pattern for the 35 investig ated elements which is similar to alpha Cir (Kupka et al. 1996, Paper I). Fe and Ni have about solar abundance, Cr and especially Co are cle arly overabundant as well as rare earth elements. The most under-abund ant element is Sc, followed by C, N, and O, which is a common property of CP2 stars. The lack of a correlation in our data between individua l line abundances and their effective Lande factors implies a mean mag netic field modulus not exceeding few kG. Compared to the last homogen eous spectroscopic investigation of a large sample of chemically pecul iar stars (21 cool Ap stars, Adelman 1973), our analysis is based on d ata with higher spectral resolution and signal-to-noise ratio. Even mo re important, we are using a much larger atomic line data base with mo re precise atomic parameters than available more than twenty years ago .