FE-RICH SOLAR ENERGETIC PARTICLE EVENTS DURING SOLAR MINIMUM

During the first 10 months of WIND observations, we have detected seve ral time periods with energetic particle abundances that are character istic of impulsive flares: enrichments in the He-3 isotope, and in hea vy ions compared to the corona. Using the Supra-Thermal through Energe tic Particle sensor on WIND, we find that at similar to 100 keV/nucleo n there events typically arrive in sequences of multiple events when t he spacecraft is magnetically connected to an active region at western solar longitudes, preceding the arrival of a high speed solar wind st ream. During recurrent high speed solar wind streams with their associ ated flux enhancements Fe-rich events are seldom seen: almost all of t he events occur on days with solar wind speeds < 450 km/sec. The impul sive events we observe arrive at a rate of similar to 30 events/year a t solar minimum for energies greater than or equal to 120 keV/nucleon. This rate is comparable to upper limits placed on the observed rate o f higher energy He-3-rich events in the last solar minimum with measur ements from ISEE-3.