  Cosmic ray particles are more rapidly accelerated in oblique shocks, with the
magnetic field inclined with respect to the shock normal direction, than in
parallel shocks, as a result of mirror reflection at the shock surface and
slower diffusion in the shock normal direction. We investigate quantitatively
how these effects contribute to reducing the acceleration time over the whole
range of magnetic field inclinations. It is shown that, for quasi-perpendicular
inclination, the mirror effect plays a remarkable role in reducing the
acceleration time; whereas, at relatively small inclination, the anisotropic
diffusion effect is dominant in reducing that time. These results are important
for a detailed understanding of the mechanism of particle acceleration by an
oblique shock in space and heliosphereic plasmas.
