CHARACTERISTIC BOUNDARY TRANSITIONS IN ENERGETIC PARTICLE DATA (60-GREATER-THAN-OR-EQUAL-TO-260 KEV) RECORDED AT COMETS P GRIGG-SKJELLERUP AND P/HALLEY BY THE EPONA INSTRUMENT ON GIOTTO/

An overview of published magnetic field, low energy electron and low t o intermediate energy ion data recorded on board Giotto during an enco unter with P/Grigg-Skjellerup (G-S) on 10 July, 1992 is presented and these measurements compared with particle data secured by the onboard energetic particles experiment EPONA (E = 60 to greater than or equal to 260 keV). It is shown that, in general, the same cometary boundarie s (Bow Wave, Bow Shock, Mystery Boundary Transitions (MBTs)) were sens ed in energetic particles as by the other experiments. Elevated fluxes of accelerated particles, interpreted to be ions of species M = 16-18 , were identified in the G-S cometosheath. It is inferred that heavy c ometary ions of species M = 28-33 were present in the innermost region of the comet (as viewed in the sunward direction). Energetic particle s recorded by EPONA on Giotto at P/Halley are considered relative to o ther particles and fields measurements obtained onboard. Evidence base d on pitch angle data indicates that, inbound, the MBTs at G-S and at Halley, were spatially associated with changes from trapped to ''flowi ng'' distributions of water group ions, suggesting that mirroring of t hese particles was taking place during encounter in the magnetic field piled up around each comet. Downstream of the MBTs, outbound, flowing distributions were, in each case, identified. Evidence of MBTs in ene rgetic particle data are, herein, reported for the first time. The rol es of various mechanisms in accelerating cometary ions in association with Bow Wave/Bow Shock boundaries at G-S and at Halley are inferred f rom comparisons between experimental and theoretical spectra pertinent to each comet. Similarities and differences between the signatures of characteristic boundaries recorded in each case are discussed in the light of basic differences between the comets themselves, and between the ambient interplanetary circumstances pertaining during each cometa ry encounter. (C) 1997 Elsevier Science Ltd.