  The Pade code has been developed to treat hydrodynamic turbulence in
protoplanetary disks. It solves the compressible equations of motion in
cylindrical coordinates. Derivatives are computed using non-diffusive and
conservative fourth-order Pade differencing, which has higher resolving power
compared to both dissipative shock-capturing schemes used in most astrophysics
codes, as well as non-diffusive central finite-difference schemes of the same
order. The fourth-order Runge-Kutta method is used for time stepping. A
previously reported error-corrected Fargo approach is used to reduce the time
step constraint imposed by rapid Keplerian advection. Artificial bulk viscosity
is used when shock-capturing is required. Tests for correctness and scaling
with respect to the number of processors are presented. Finally, efforts to
improve efficiency and accuracy are suggested.
