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The Kerr metric that describes the spacetime of a spinning supermassive blackhole (SMBH) is axisymmetric, implying that the nearly parabolic geodesics onwhich stars approach the SMBH depend on the inclination angle $\iota$ of theorbital angular momentum with respect to the SMBH spin. This inclinationaffects both the geodesic deviation that determines whether a star is tidallydisrupted and whether the tidal debris survives direct capture by the eventhorizon to produce an observable tidal disruption event (TDE). The steady-stateTDE rate is the rate at which stars are scattered into the loss cone determinedby these spin- and inclination-dependent effects. As the anisotropy of thisloss-cone refilling is highly uncertain, we consider the two extreme limits inwhich stellar inclination is preserved (IP) or isotropized (ISO). We calculatethe inclination distribution in these two limits and find a prograde bias inthe 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 whenthe empty loss cone suppresses capture and allows the weaker retrograde bias ofgeodesic deviation to dominate. We also calculate the total TDE rates andmaximum SMBH mass $M_{\rm \bullet, max}$ for tidal disruption in these twolimits. In the IP limit, we find a highly spin-dependent capture cutoff in theTDE rate and $M_{\rm \bullet, max} \approx 10^{8.45} M_\odot$ for maximal SMBHspin. In the ISO limit, we find a strong spin-dependent enhancement in the TDErate at intermediate SMBH masses, a weakly spin-dependent capture cutoff above$M_\bullet \approx 10^{7.5} M_\odot$, and $M_{\rm \bullet, max} \approx10^{7.95} M_\odot$ for maximal SMBH spin.

Distribution of orbital inclinations for tidal disruption events by Kerr black holes