E.W. Cliver
      Air Force Research Laboratory, Hanscom AFB, Massachusetts, USA 

The gamma-ray-line (GRL)observations from the the Gamma Ray Spectrometer (GRS) on the Solar Maximum Mission (SMM) made it possible for the first time to compare the numbers and compositions of ions interacting at the Sun during the times of solar flares with those of the particles subsequently observed in space. Previously (Cliver et al., Astrophys. J. 343, 953, 1989), we reported that the prompt 4-8 MeV GRL fluences from flares were poorly correlated with the peak fluxes of 10 MeV interplanetary proton events. The earlier study was based on data from the first half of the SMM lifetime (1980-1985). Here I report on an update of this comparison (undertaken with T. Vestrand and D. Reames) that extends to the end of SMM GRS observations in late 1989. I also review work by others that compares the composition of interacting particles with those observed in space. The various results are discussed in terms of the two-class picture of solar energetic particle events.