Differences in proton fluxes near the earth from solar coronal mass ejections of different origin

We investigate proton fluxes at energies E in the range from 50 keV to 100 MeV, which accompany coronal mass ejections (CME) during filament disappear ances (five events) and during proton (two events) and non-proton (two even ts) flares. We show that. when large H-alpha filaments disappear, the proto n flux at E less than or equal to 1.8 MeV can be no weaker than the flux du ring proton flares. In this case, however, the proton flux at E > 10 MeV du ring filament disappearances is much lower than its value during proton eve nts. We propose a method of determining differences in the spectra of proto ns from CMEs of different origin from changes in the slope of the proton sp ectrum during an event relative to the slope of the undisturbed background proton spectrum near the event. The flattening of the proton spectrum with increasing energy during proton events, which is absent during non-proton e vents and filament disappearances, suggests that there is a peculiar mechan ism for the emergence of energetic particles in proton flares.