Solar electron events are common phenomenon observed in interplanetary space. Electrons from < 1 keV to > 300 keV are often observed in these events with an occurrence rate near the earth of ∼ 190 events per year during solar maximum and ∼ 10 per year during solar minimum [Wang et al., 2012]. In many of these
events 3He ions are also observed at a significantly enhanced level. A majority of these events is related to small flares and they have no fast coronal mass ejections (CMEs) associated with them. Thus the underlying acceleration process is confined both spatially and temporally. Once they are accelerated and escape from the Sun, high energy electrons and ions propagate along the interplanetary magnetic field and scatter off various plasma waves. Observational characteristics (time intensity profiles and spectra) of these electrons and ions provide a probe of the configuration and turbulence level of the interplanetary magnetic field. Recent observations from multiple spacecraft (e.g. STEREO-A/B, Wind, and ACE) showed that electrons and ions in many of these events can be observed over a longitudinal separation of > 90 degrees or larger. What causes these large separations? Could it be due to large cross field diffusion or due to significant field line meandering, or perhaps the magnetic field near the Sun experiences a significant divergence within a few solar radii? To answer these questions, we propose a comprehensive investigation which includes both observations and simulations, to be carried out by a group of experts in solar and heliospheric theory,
modelling, and observations. With these combined studies, we aim to reveal the interplanetary magnetic field configuration in solar electron events. We will also quantify the solar wind turbulence level in these events through numerical simulation, obtain particle mean free paths; and using the resulting mean free path parameter to classify events into scatter-free and scatter-dominated cases. We will construct an event
database which can be used by the heliospheric community. We have collected a team with significant expertise in solar and heliospheric modelling, theory, observations and instrumentation. Such a diverse team will allow successful execution of the proposed study.