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We present axisymmetric numerical simulations of radiatively inefficientaccretion flows onto black holes combining general relativity,magnetohydrodynamics, self-consistent electron thermodynamics, andfrequency-dependent radiation transport. We investigate a range of accretionrates up to $10^{-5} \dot{M}_{\mathrm{Edd}}$ onto a $10^8 M_{\odot}$ black holewith spin $a_{\star} = 0.5$. We report on averaged flow thermodynamics as afunction of accretion rate. We present the spectra of outgoing radiation andfind that it varies strongly with accretion rate, from synchrotron-dominated inthe radio at low $\dot{M}$ to inverse Compton-dominated at our highest$\dot{M}$. In contrast to canonical analytic models, we find that by $\dot{M}\approx 10^{-5} \dot{M}_{\mathrm{Edd}}$, the flow approaches $\sim 1\%$radiative efficiency, with much of the radiation due to inverse Comptonscattering off Coulomb-heated electrons far from the black hole. These resultshave broad implications for modeling of accreting black holes across a largefraction of the accretion rates realized in observed systems.

The Radiative Efficiency and Spectra of Slowly Accreting Black Holes from Two-Temperature GRRMHD Simulations