Energy spectra of 50-keV to 20-MeV protons accelerated at corotating interaction regions at Ulysses

We analyze here the energy spectra of 50-keV to 20-MeV protons accelerated at corotating shocks observed at Ulysses in the southern heliosphere during 1992 and 1993. In general, our results are inconsistent with the predictio ns of two models based on diffusive shock acceleration theory (Fisk and Lee [1980] and Jones and Ellison [1991]). The main results are the following: (1) The relationships between the spectral indices and the shock compressio n ratio show significant departures from those predicted by the two models; the observed spectra are substantially harder than predicted; (2) the spec tral indices at the reverse shocks depend strongly on the heliographic lati tude of Ulysses; the hardest spectra are associated with strong quasi-perpe ndicular shocks observed between 20 degrees S and 30 degrees S; (3) the spe ctral indices at the reverse shocks are anticorrelated with the upstream pl asma velocity V-u' in the de Hoffman-Teller frame of the shock; and (4) the spectral indices at the forward shocks show no dependence on either the sh ock parameters or the heliographic latitude. The latitudinal dependence of the reverse shock spectra is probably related to the tilt (similar to 25 de grees) of the heliospheric current sheet with respect to the solar equatori al plane during 1992 and 1993. The negative correlation between the spectra l indices at the reverse shocks and V-u' indicates that the gradient drift mechanism plays a crucial role in accelerating particles at corotating inte raction regions (CIRs). The differences in our observations at the forward and reverse shocks may be due to the presence of a more energetic seed popu lation and an enhancement in the level of magnetic field fluctuations upstr eam of the trailing edges of the CIRs.