  We develop a semi-analytic method for determining the phase-space population
of tidal debris along the orbit of a disrupting satellite galaxy and illustrate
its use with a number of applications. We use this method to analyze Zhao's
proposal that the microlensing events towards the Large Magellanic Cloud (LMC)
might be explained by an appropriately placed tidal streamer, and find that his
scenarios lead either to unacceptably high overdensities (10 -- 100%) in faint
star counts (apparent magnitudes 17.5 -- 20.5) away from the Galactic plane or
short timescales for the debris to disperse (10^8 years). We predict that the
tidal streamers from the LMC and the Sagittarius dwarf galaxy currently extend
over more than $2\pi$ in azimuth along their orbits. Assuming that each
satellite has lost half of its primordial mass, we find that the streamers will
have overdensities in faint star counts of 10 -- 100% and < 1% respectively,
and conclude that this mass loss rate is unlikely for the LMC, but possible for
Sagittarius. If the Galaxy has accreted one hundred $10^5-10^6 M_{\odot}$
objects (comparable to its current population of globular clusters) at
distances of 20 -- 100 kpc during its lifetime then 10% of the sky will now be
covered by tidal streamers.
