SIMBAD references

We apply the one dimensional version of the multi-dimensional robust solver developed by Hujeirat & Rannacher to follow the viscous evolution of various models of polytropic boundary layers in accretion disks around a non-magnetic white dwarf. In this paper, we present the results of 13 different time-dependent hydrodynamical calculations. The results indicate that 1) no steady structure of the flow in the boundary layer is encountered. The solutions show that a quasi-standing shock is always present for very small α and high stellar rotation, 2) the rate of accreted angular momentum into the central object is much less than the corresponding Keplerian one, 3) the radial extent of the boundary layer (δR^BL) is much smaller than the vertical one as well as the radial extent of classical viscous boundary layers, 4) δR^BL increases with the rotational speed of the star, 5) an instability of the shock position is detected as well as quasi-periodic oscillations which are viscosity-dependent, 6) the polytropic equation of state with γ=2 yields unstable and chaotic behaviour of the flow in the disk region.