In an attempt to model the accretion onto a neutron star in low-mass X-ray binaries , we present two-dimensional hydrodynamical models of the gas flow in close vicinity of the stellar surface .
First we consider a gas pressure dominated case , assuming that the star is non-rotating .
For the stellar mass we take M _ { star } = 1.4 \times 10 ^ { -2 } { M _ { \odot } } and for the gas temperature T = 5 \times 10 ^ { 6 } K. Our results are qualitatively different in the case of a realistic neutron star mass and a realistic gas temperature of T \simeq 10 ^ { 8 } K , when the radiation pressure dominates .
We show that to get the stationary solution in a latter case , the star most probably has to rotate with the considerable velocity .