  We have performed a series of two-dimensional two-temperature general
relativistic magnetohydrodynamic simulations of magnetized accretion flows
initiated from tori with different sizes and poloidal magnetic loop polarities.
In these two temperature simulations, we trace the process of heating electrons
through turbulence and reconnection, most of the time these electrons are
trapped in plasmoids. We found that the accretion process strongly depends on
the size of the magnetic loops. The accretion flows never reach the
magnetically arrested (MAD) regime in small loop cases. Interaction between
magnetic field with different polarities dissipates and decreases the
efficiency of magneto-rotational instability. The dependency on the wavelength
of the loops places a lower limit on the loop size. In the large loop cases,
after reaching a quasi-steady phase, a transition from Standard And Normal
Evolution (SANE) flow to MAD flow is observed. The transition of the accretion
state and the transition time depends on the initial loop wavelength. The
formation of plasmoids strongly depends on the size of the magnetic loops. The
frequent magnetic reconnection between the magnetic loops is responsible for
the formation of most of the plasmoids. For some plasmoids, Kelvin-Helmholtz
and tearing instabilities are coexisting, showing another channel of plasmoid
formation. The simulations present that electrons in the plasmoids are
well-heated up by turbulent and magnetic reconnection. Different properties of
plasmoid formation in different magnetic field configurations provide new
insights for the understanding of flaring activity and electron thermodynamics
in Sgr A*.
