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

¹ Institute of Space Physics and Applied Technology, 100871 Beijing, PR China
e-mail: wanglhwang@gmail.com
² Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA
³ Institute of 4D Technologies, University of Applied Sciences Northwestern Switzerland, 5210 Windisch, Switzerland
⁴ Applied Physics Laboratory, Johns Hopkins University, Laurel, MD 20723, USA
⁵ Department of Space Science and CSPAR, University of Alabama in Huntsville, Huntsville, AL 35899, USA

Received: 29 August 2015
Accepted: 2 November 2015

Abstract

We have derived the particle injections at the Sun for ten good electron/³He-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 ± 3 min 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 R_S, 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.