  We study tidal effects on self-gravitating Newtonian stars rotating around a
Kerr black hole in stable circular orbits away from the equatorial plane. Such
cases are exemplified by a non-vanishing Carter's constant. Here, we calculate
the tidal disruption limit (Roche limit) of the star numerically, in Fermi
normal coordinates. The Roche limit is found to depend strongly on the choice
of the orbit, and differs significantly from the equatorial plane result as one
approaches nearly polar orbits. As expected, this difference is large when the
star is close to the black hole (near to the innermost stable circular orbit)
and becomes smaller when the star is far from it. We also discuss the
dependence of the Roche limit on the equation of state of the star, taking two
specific parameter values as examples.
