Observations at 1 au have confirmed that enhancements in measured energetic particle uxes are sta-tistically associated with rough" magnetic fields, i.e., fields having atypically large spatial derivatives or increments, as measured by the Partial Variance of Increments (PVI) method. One way to interpret this observation is as an association of the energetic particles with trapping or channeling within mag-netic ux tubes, possibly near their boundaries. However, it remains unclear whether this association is a transport or local effect; i.e., the particles might have been energized at a distant location, perhaps by shocks or reconnection, or they might experience local energization or re-acceleration. The Parker Solar Probe (PSP), even in its first two orbits, offers a unique opportunity to study this statistical correlation closer to the corona. As a first step, we analyze the separate correlation properties of the energetic particles measured by the ISfiIS instruments during the first solar encounter. The distribu-tion of time intervals between a specific type of event, i.e., the waiting time, can indicate the nature of the underlying process. We find that the ISfiIS observations show a power-law distribution of waiting times, indicating a correlated (non-Poisson) distribution. Analysis of low-energy ISfiIS data suggests that the results are consistent with the 1 au studies, although we find hints of some unexpected be-havior. A more complete understanding of these statistical distributions will provide valuable insights into the origin and propagation of solar energetic particles, a picture that should become clear with future PSP orbits.
|Original language||English (US)|
|State||Published - Dec 6 2019|
- (Sun:) Solar Wind
- Acceleration Of Particles
ASJC Scopus subject areas