  We present the first-ever moving-mesh general relativistic hydrodynamics
solver for static spacetimes as implemented in the code, MANGA. Our
implementation builds on the architectures of MANGA and the numerical
relativity Python package NRPy+. We review the general algorithm to solve these
equations and, in particular, detail the time stepping; Riemann solution across
moving faces; conversion between primitive and conservative variables;
validation and correction of hydrodynamic variables; and mapping of the metric
to a Voronoi moving-mesh grid.
  We present test results for the numerical integration of an unmagnetized
Tolman-Oppenheimer-Volkoff star for 24 dynamical times. We demonstrate that at
a resolution of $10^6$ mesh generating points, the star is stable and its
central density drifts downward by 2% over this timescale. At a lower
resolution the central density drift increases in a manner consistent with the
adopted second order spatial reconstruction scheme. These results agree well
with the exact solutions, and we find the error behavior to be similar to
Eulerian codes with second-order spatial reconstruction. We also demonstrate
that the new code recovers the fundamental mode frequency for the same TOV star
but with its initial pressure depleted by 10%
