The injection of ten electron/3He-rich SEP events

We have derived the particle injections at the Sun for ten good electron/ 3 He-rich solar energetic particle (SEP) events, using a 1.2 AU particle path length (suggested by analysis of the velocity dispersion). The inferred solar injections of high-energy (∼10 to 300 keV) electrons and of ∼MeV/nucleon ions (carbon and heavier) start with a delay of 17 ± 3m in and 75± 14 min, respectively, after the injection of low-energy (∼0.4 to 9 keV) electrons. The injection duration (averaged over energy) ranges from ∼200 to 550 min for ions, from ∼90 to 160 min for low-energy electrons, and from ∼10 to 30 min for high-energy electrons. Most of the selected events have no reported Hα flares or GOES SXR bursts, but all have type III radio bursts that typically start after the onset of a low-energy electron injection. All nine events with SOHO/LASCO coverage have a relatively fast (>570 km s −1 ), mostly narrow (30 ◦ ), west-limb coronal mass ejection (CME) that launches near the start of the low-energy electron injection, and reaches an average altitude of ∼1.0 and 4.7 RS, respectively, at the start of the high-energy electron injection and of the ion injection. The electron energy spectra show a continuous power law extending across the transition from low to high energies, suggesting that the low-energy electron injection may provide seed electrons for the delayed high-energy electron acceleration. The delayed ion injections and high ionization states may suggest an ion acceleration along the lower altitude flanks, rather than at the nose of the CMEs.