THE STRUCTURE OF THE ACCRETION DISC BOUNDARY-LAYER AROUND A ROTATING,NON-MAGNETIZED STAR

The process of disc accretion onto rotating nonmagnetized stars is con sidered. Closed system of equations is written for the boundary layer which exists between Keplerian outer part of the disc and more slowly rotating star surface. Under certain simplifying assumptions the syste m is solved numerically for main physical variables. Energy conservati on equation is used for finding the boundary layer radiation intensity . The results are discussed with a special emphasize on their importan ce as well as on possible shortcomings.