  Magnetorotational Instability (MRI), the instability causing turbulent
transport in accretion disks, is studied in the kinetic regime. Radiatively
Inefficient Accretion Flows (RIAFs), like the one around the supermassive black
hole in the center of our Galaxy, are believed to be collisionless. Kinetic MHD
formalism, based on the moments of the Vlasov equation, is used for linear
analysis and nonlinear simulations.
  ZEUS MHD code is modified to include key kinetic MHD terms: anisotropic
pressure tensor and anisotropic thermal conduction. Simulations use the local
shearing box approximation. Pressure anisotropy is created, because of the
adiabatic invariance ($\mu=p_\perp/B$), as magnetic field is amplified by the
MRI. Larmor radius scale instabilities--mirror, ion-cyclotron, and
firehose--are excited at large pressure anisotropy. Pressure isotropization due
to pitch angle scattering by these instabilities is included as a subgrid
model. A key result of the kinetic MHD simulations is that the anisotropic
(viscous) stress can be as large as the Maxwell stress.
  A new numerical method to simulate anisotropic thermal conduction with large
temperature gradients is suggested. Simple tests show that the centered
differencing of anisotropic thermal conduction can result in heat flowing from
lower to higher temperatures, giving rise to negative temperatures. Limiting of
transverse temperature gradients does not accentuate temperature extrema.
