  We present two-dimensional general relativistic radiative
magnetohydrodynamical simulations of accretion disks around non-rotating
stellar-mass black hole. We study the evolution of an equilibrium accreting
torus in different grid resolutions to determine an adequate resolution to
produce a stable turbulent disk driven by magneto-rotational instability. We
evaluate the quality parameter, $Q_{\theta}$, from the ratio of MRI wavelength
to the grid zone size and examine the effect of resolution in various
quantitative values such as the accretion rate, magnetisation, fluxes of
physical quantities and disk scale-height. We also analyse how the resolution
affects the formation of plasmoids produced in the magnetic reconnection
events.
