  We present first results from a new technique for the prediction of Fe
K$\alpha$ profiles directly from general relativistic magnetohydrodynamic
(GRMHD) simulations. Data from a GRMHD simulation are processed by a Monte
Carlo global radiation transport code, which determines the X-ray flux
irradiating the disk surface and the coronal electron temperature
self-consistently. With that irradiating flux and the disk's density structure
drawn from the simulation, we determine the reprocessed Fe K$\alpha$ emission
from photoionization equilibrium and solution of the radiation transfer
equation. We produce maps of the surface brightness of Fe K$\alpha$ emission
over the disk surface, which---for our example of a $10 M_\odot$, Schwarzschild
black hole accreting at $1\%$ the Eddington value---rises steeply one
gravitational radius outside the radius of the innermost stable circular orbit
and then falls $\propto r^{-2}$ at larger radii. We explain these features of
the Fe K$\alpha$ radial surface brightness profile as consequences of the
disk's ionization structure and an extended coronal geometry, respectively. We
also present the corresponding Fe K$\alpha$ line profiles as would be seen by
distant observers at several inclinations. Both the shapes of the line profiles
and the equivalent widths of our predicted K$\alpha$ lines are qualitatively
similar to those typically observed from accreting black holes. Most
importantly, this work represents a direct link between theory and observation:
in a fully self-consistent way, we produce observable results---iron
fluorescence line profiles---from the theory of black hole accretion with
almost no phenomenological assumptions.
