  Non-ideal MHD effects may play a significant role in determining the
dynamics, thermal properties, and observational signatures of radiatively
inefficient accretion flows onto black holes. In particular, particle
acceleration during magnetic reconnection events may influence black hole
spectra and flaring properties. We use representative GRMHD simulations of
black hole accretion flows to identify and explore the structures and
properties of current sheets as potential sites of magnetic reconnection. In
the case of standard and normal (SANE) disks, we find that, in the reconnection
sites, the plasma beta ranges from $0.1$ to $1000$, the magnetization ranges
from $10^{-4}$ to $1$, and the guide fields are weak compared to the
reconnecting fields. In magnetically arrested (MAD) disks, we find typical
values for plasma beta from $10^{-2}$ to $10^3$, magnetizations from $10^{-3}$
to $10$, and typically stronger guide fields, with strengths comparable to or
greater than the reconnecting fields. These are critical parameters that govern
the electron energy distribution resulting from magnetic reconnection and can
be used in the context of plasma simulations to provide microphysics inputs to
global simulations. We also find that ample magnetic energy is available in the
reconnection regions to power the fluence of bright X-ray flares observed from
the black hole in the center of the Milky Way.
