  We present the results the photometric observations of the Type IIP supernova
SN 2012aw obtained for the time interval from 7 till 371 days after the
explosion. Using the previously published values of the photospheric velocities
we've computed the hydrodynamic model which simultaneously reproduced the
photometry observations and velocity measurements. The model was calculated
with the multi-energy group radiation hydrodynamics code STELLA. We found the
parameters of the pre-supernova: radius $R = 500 R_\odot$, nickel mass
$M(^{56}$Ni$)$ $\sim 0.06 M_\odot$, pre-supernova mass $25 M_\odot$, mass of
ejected envelope $23.6 M_\odot$, explosion energy $E \sim 2 \times 10^{51}$
erg. The model progenitor mass $M=25 M_\odot$ significantly exceeds the upper
limit mass $M=17 M_\odot$, obtained from analysis the pre-SNe observations.
This result confirms once more that the 'Red Supergiant Problem' must be
resolved by stellar evolution and supernova explosion theories in interaction
with observations.
