  The Kerr metric that describes the spacetime of a spinning supermassive black
hole (SMBH) is axisymmetric, implying that the nearly parabolic geodesics on
which stars approach the SMBH depend on the inclination angle $\iota$ of the
orbital angular momentum with respect to the SMBH spin. This inclination
affects both the geodesic deviation that determines whether a star is tidally
disrupted and whether the tidal debris survives direct capture by the event
horizon to produce an observable tidal disruption event (TDE). The steady-state
TDE rate is the rate at which stars are scattered into the loss cone determined
by these spin- and inclination-dependent effects. As the anisotropy of this
loss-cone refilling is highly uncertain, we consider the two extreme limits in
which stellar inclination is preserved (IP) or isotropized (ISO). We calculate
the inclination distribution in these two limits and find a prograde bias in
the IP limit because of the strong retrograde bias for direct capture. However,
we find a retrograde bias in the ISO limit for intermediate SMBH masses when
the empty loss cone suppresses capture and allows the weaker retrograde bias of
geodesic deviation to dominate. Partially empty loss cones lead to steeper
distributions of the penetration factor $\beta$ than for a full loss cone, with
this effect even more pronounced in the ISO limit. We also calculate the total
TDE rates and maximum SMBH mass $M_{\rm \bullet, max}$ for tidal disruption in
these two limits. In the IP limit, we find a highly spin-dependent capture
cutoff in the TDE rate and $M_{\rm \bullet, max} \approx 10^{8.45} M_\odot$ for
maximal SMBH spin. In the ISO limit, we find a strong spin-dependent
enhancement in the TDE rate at intermediate SMBH masses, a weakly
spin-dependent capture cutoff above $M_\bullet \approx 10^{7.5} M_\odot$, and
$M_{\rm \bullet, max} \approx 10^{7.95} M_\odot$ for maximal SMBH spin.
