  We describe how the various outcomes of stellar tidal disruption give rise to
observable radiation. We separately consider the cases where gas circularizes
rapidly into an accretion disc, as well as the case when shocked debris streams
provide the observable emission without having fully circularized. For the
rapid circularization case, we describe how outflows, absorption by
reprocessing layers, and Comptonization can cause the observed radiation to
depart from that of a bare disc, possibly giving rise to the observed
optical/UV emission along with soft X-rays from the disc. If, instead, most of
the debris follows highly eccentric orbits for a significant time, many
properties of the observed optical/UV emission can be explained by the scale of
those eccentric orbits and the shocks embedded in the debris flow near orbital
apocenter. In this picture, soft X-ray emission at early times results from the
smaller amount of debris mass deflected into a compact accretion disc by weak
shocks near the stellar pericenter. A general proposal for the near-constancy
of the ultraviolet/optical color temperatures is provided, by linking it to
incomplete thermalization of radiation in the atmosphere of the emitting
region. We also briefly discuss the radio signals from the interaction of
unbound debris and jets with the black hole environment.
