  We perform axisymmetric, two-dimensional magnetohydrodynamic (MHD)
simulations to investigate accretion flows around spinning AGN. To mimic the
space-time geometry of spinning black holes, we consider effective Kerr
potential, and the mass of the black holes is $10^8 M_{\odot}$. We initialize
the accretion disc with a magnetized torus by adopting the toroidal component
of the magnetic vector potential. The initial magnetic field strength is set by
using the plasma beta parameter ($\beta_0$). We observe self-consistent
turbulence generated by magneto rotational instability (MRI) in the disc. The
MRI turbulence transports angular momentum in the disc, resulting in an angular
momentum distribution that approaches a Keplerian distribution. We investigate
the effect of the magnetic field on the dynamics of the torus and associated
mass outflow from the disc around a maximally spinning black hole $(a_k =
0.99)$. For the purpose of our analysis, we investigate the magnetic state of
our simulation model. The model $\beta_0 = 10$ indicates the behaviour similar
to the "magnetically arrested disk (MAD)'' state, and all the other low
magnetic model remains in the SANE state. We observe that mass outflow rates
are significantly enhanced with the increased magnetic field in the disc. We
find a positive correlation between the magnetic field and mass outflow rates.
We also investigate the effect of black hole spin on the magnetized torus
evolution. However, we have not found any significant effect of black hole spin
on mass outflows in our model. Finally, we discuss the possible astrophysical
applications of our simulation results.
