Spectrum of the star BM Ori at minimum light

Two spectra of the star BM Ori were obtained with the 2.6-m Crimean Astroph ysical Observatory telescope near its maximum eclipse phase. The light dete ctor was a CCD array. The wavelength range 5305-5373 A was chosen in such a way that it contained no strong primary lines. Optimum filtration of the s pectra yielded a signal-to-noise ratio of similar to 300. Eighteen secondar y lines are seen in the spectrum. Atmospheric parameters of the secondary s tar were determined: T-eff = 5740 K and logg = 3.0; the secondary was class ified by these parameters as being of spectral type G2 III. The best agreem ent between observed and synthetic spectra is achieved for metallicity [M/H ] = -0.5 and microturbulence xi(t) = 0 km s(-1). The projected rotational v elocity is Vsini = 60 km s(-1), in agreement with the synchronous velocity in the hypothesis that assumes a total eclipse by the secondary star. Atmos pheric elemental abundances in the secondary are estimated. Nickel, chromiu m, and iron exhibit an underabundance of similar to 1 dex, (C) 2000 MAIK "N auka/Interperiodica".