  Since the collisional mean free path of charged particles in hot accretion
flows can be significantly larger than the typical length-scale of the
accretion flows, the gas pressure is anisotropic to magnetic field lines. For
such a large collisional mean free path, the resistive dissipation can also
play a key role in hot accretion flows. In this paper, we study the dynamics of
resistive hot accretion flows in the presence of anisotropic pressure. We
present a set of self-similar solutions where the flow variables are assumed to
be a function only of radius. Our results show that the radial and rotational
velocities and the sound speed increase considerably with the strength of
anisotropic pressure. The increase in infall velocity and in sound speed are
more significant if the resistive dissipation is taken into account. We find
that such changes depend on the field strength. Our results indicate that the
resistive heating is $10\%$ of the heating by the work done by anisotropic
pressure when the strength of anisotropic pressure is 0.1. This value becomes
higher when the strength of anisotropic pressure reduces. The increase in disk
temperature can lead to heating and acceleration of the electrons in such
flows. It helps us to explain the origin of phenomena such as the flares in
Galactic Center Sgr A*.
