  We study the distribution of accretion rates onto supermassive black holes
(SMBH) in AGNs of the local Universe ($z<0.15$) based on near-infrared and hard
X-ray surveys (2MASS and Swift/BAT). Using sufficiently accurate black hole
mass estimates, we reliably estimated the Eddington ratio, $\lambda_{Edd}$, for
approximately half of the objects in the AGN sample; for the remaining ones we
used a rougher estimate based on the correlation of $M_{BH}$ with the galaxy
stellar mass $M_\ast$. We found that for a wide range of galaxy masses,
$9.28<\log(M_\ast/M_\odot)<12.28$, including the most massive galaxies in the
local Universe, the distribution $f(\lambda_{Edd})$ above
$\log{\lambda_{Edd}}=-3$ can be described by a power law with
$M_\ast$-independent parameters, declining with a characteristic slope $\approx
0.7$ up to the Eddington limit ($\log{\lambda_{Edd}}\sim 0$), where there is
evidence for a break. In addition, there is evidence that at
$\log{\lambda_{Edd}}<-3$ the dependence $f(\lambda_{Edd})$ has a lower slope or
flattens out. The mean characteristic growth time of SMBHs at the present epoch
turns out to depend weakly on the galaxy stellar mass and to exceed the
lifetime of the Universe but by no more than one order of magnitude. The mean
duty cycle of SMBHs (the fraction of objects with $\lambda_{Edd}>0.01$) in the
local Universe also depends weakly on $M_\ast$ and is 0.2-1%. These results
confirm the trends found in previous studies for the earlier Universe and
refine the parameters of the dependence $f(\lambda_{Edd}|M_\ast)$ at $z<0.15$.
The revealed universal (weakly dependent on the galaxy stellar mass) pattern of
the dependence $f(\lambda_{Edd})$ probably stems from the fact that, at
present, the episodes of mass accretion onto SMBHs are associated mainly with
stochastic processes in galactic nuclei rather than with global galaxy
evolution processes.
