1 Introduction

Knowledge of the astrophysical parameters of the stellar atmospheres (i.e., $T_{\mathrm{eff}}$, $\log g$,[A/H], $v_{\mathrm{turb}}$) of any given star is crucial for many fields of modern astrophysics. Recent developments in model atmosphere computation and significant increase in computer speeds make a global approach to this problem possible. Parameters of the model atmosphere and the synthetic spectra can be fit to match observed spectra.

Recently published works on spectrum fitting (e.g. Cuisinier et al. 1994) apply a pretabulated grid of synthetic spectra (see Barbuy et al. 1990; Cayrel et al. 1991 for spectra with lower resolving power, Chavez et al. 1997 for spectra with higher resolving power). Our method does not employ any pretabulated grid of synthetic spectra, but we do compute synthetic spectra using the appropriate model atmosphere in different wavelength intervals. A spectral region less crowded by lines (in the red part of spectrum) leads to more accurate determination of the continuum position. A similar approach was proposed by some authors with automatic codes: MERSEN (Cowley 1996), SME (Valenti & Piskunov 1996) and some others.