  Triaxial neutron stars can be sources of continuous gravitational radiation
detectable by ground-based interferometers. The amplitude of the emitted
gravitational wave can be greatly affected by the state of the hydrodynamical
fluid flow inside the neutron star. In this work we examine the most triaxial
models along two sequences of constant rest mass, confirming their dynamical
stability. We also study the response of a triaxial figure of quasiequilibrium
under a variety of perturbations that lead to different fluid flows. Starting
from the general relativistic compressible analog of the Newtonian Jacobi
ellipsoid, we perform simulations of Dedekind-type flows. We find that in some
cases the triaxial neutron star resembles a Riemann-S-type ellipsoid with minor
rotation and gravitational wave emission as it evolves towards axisymmetry. The
present results highlight the importance of understanding the fluid flow in the
interior of a neutron star in terms of its gravitational wave content.
