  We address the problem of deconvolving the effects of interplanetary
transport on observed intensity and anisotropy profiles of solar energetic
particles with the goal of determining the time profile and spectrum of
particle injection near the Sun as well as the interplanetary scattering mean
free path. Semi-automated techniques have been developed to quantitatively
determine the best fit injection profile, assuming (1) a general piecewise
linear profile or (2) a Reid profile of the form
[C/(t-t_0)]exp[-A/(t-t_0)-(t-t_0)/B]. The two assumptions for the form of the
injection profile yielded similar results when we tested the techniques using
ISEE 3 proton data from the solar flare events of July 20, 1981 (gradual
flare), and January 2, 1982 (impulsive flare). For the former event, the
duration of injection was much shorter for protons of higher energy (75-147
MeV), which may be interpreted as indicating that the coronal mass
ejection-driven shock lost the ability to accelerate protons to $\sim$100 MeV
after traveling beyond a certain distance from the Sun.
