  The velocity, position, and action variable evolution of a tidal stream drawn
out of a star cluster in a triaxial isochrone potential containing a sub-halo
population reproduces many of the orbital effects of more general cosmological
halos but allows easy calculation of orbital actions. We employ a spherical
shell code which we show accurately reproduces the results of a tree gravity
code for a collisionless star cluster. Streams from clusters on high
eccentricity orbits, $e\gtrsim 0.6$, can spread out so much that the amount of
material at high enough surface density to stand out on the sky may be only a
few percent of the stream's total mass. Low eccentricity streams remain more
spatially coherent, but sub-halos both broaden the stream and displace the
centerline with details depending on the orbits allowed within the potential.
Overall, the majority of stream particles have changes in their total actions
of only 1-2\%, leaving the mean stream relatively undisturbed. A halo with 1\%
of the mass in sub-halos typically spreads the velocity distribution about a
factor of two wider than would be expected for a smooth halo. Strong density
variations, "gaps", along with mean velocity offsets, are clearly detected in
low eccentricity streams for even a 0.2\% sub-halo mass fraction. Around one
hundred velocity measurements per kiloparsec of stream will enable tests for
the presence of a local sub-halo density as small as 0.2-0.5\% of the local
mass density, with about 1\% predicted for 30 kiloparsec orbital radii streams.
