Dynamical Properties of Collisionless Star Streams
  A sufficiently extended satellite in the tidal field of a host galaxy loses
mass to create nearly symmetric leading and trailing tidal streams. We study
the case in which tidal heating drives mass loss from a low mass satellite. The
stream effectively has two dynamical components, a common angular momentum core
superposed with episodic pulses with a broader angular momentum distribution.
The pulses appear as spurs on the stream, oscillating above and below the
stream centerline, stretching and blurring in configuration space as they move
away from the cluster. Low orbital eccentricity streams are smoother and have
less differential motion than high eccentricity streams. The tail of a high
eccentricity stream can develop a fan of particles which wraps around at
apocenter in a shell feature. We show that scaling the essentially stationary
action-angle variables with the cube root of the satellite mass allows a low
mass satellite stream to accurately predict the features in the stream from a
satellite a thousand times more massive. As a practical astrophysical
application, we demonstrate that narrow gaps in a moderate eccentricity stream,
such as GD-1, blur out to 50\% contrast over approximately 6 radial periods. A
high eccentricity stream, such as Pal~5, will blur small gaps in only radial 2
orbits as can be understood from the much larger dispersion of angular momentum
in the stream.
