  In the collisionless plasmas of radiatively inefficient accretion flows,
heating and acceleration of ions and electrons is not well understood. Recent
studies in the gyrokinetic limit revealed the importance of incorporating both
the compressive and Alfvenic cascades when calculating the partition of
dissipated energy between the plasma species. In this paper, we use a covariant
analytic model of the accretion flow to explore the impact of compressive and
Alfvenic heating, Coulomb collisions, compressional heating, and radiative
cooling on the radial temperature profiles of ions and electrons. We show that,
independent of the partition of heat between the plasma species, even a small
fraction of turbulent energy dissipated to the electrons makes their
temperature scale with a virial profile and the ion-to-electron temperature
ratio smaller than in the case of pure Coulomb heating. In contrast, the
presence of compressive cascades makes this ratio larger because compressive
turbulent energy is channeled primarily into the ions. We calculate the
ion-to-electron temperature in the inner accretion flow for a broad range of
plasma properties, mass accretion rates, and black hole spins and show that it
ranges between $5 \lesssim T_i/T_e \lesssim 40$. We provide a physically
motivated expression for this ratio that can be used to calculate observables
from simulations of black hole accretion flows for a wide range of conditions.
