Observations of Energetic-Particle Population Enhancements along Intermittent Structures near the Sun from Parker Solar Probe. (arXiv:1912.03424v1 [physics.space-ph])

Observations of Energetic-Particle Population Enhancements along Intermittent Structures near the Sun from Parker Solar Probe. (arXiv:1912.03424v1 [physics.space-ph])
<a href="http://arxiv.org/find/physics/1/au:+Bandyopadhyay_R/0/1/0/all/0/1">Riddhi Bandyopadhyay</a>, <a href="http://arxiv.org/find/physics/1/au:+Matthaeus_W/0/1/0/all/0/1">W. H. Matthaeus</a>, <a href="http://arxiv.org/find/physics/1/au:+Parashar_T/0/1/0/all/0/1">T. N. Parashar</a>, <a href="http://arxiv.org/find/physics/1/au:+Chhiber_R/0/1/0/all/0/1">R. Chhiber</a>, <a href="http://arxiv.org/find/physics/1/au:+Ruffolo_D/0/1/0/all/0/1">D. Ruffolo</a>, <a href="http://arxiv.org/find/physics/1/au:+Goldstein_M/0/1/0/all/0/1">M. L. Goldstein</a>, <a href="http://arxiv.org/find/physics/1/au:+Maruca_B/0/1/0/all/0/1">B. A. Maruca</a>, <a href="http://arxiv.org/find/physics/1/au:+Chasapis_A/0/1/0/all/0/1">A. Chasapis</a>, <a href="http://arxiv.org/find/physics/1/au:+Qudsi_R/0/1/0/all/0/1">R. Qudsi</a>, <a href="http://arxiv.org/find/physics/1/au:+McComas_D/0/1/0/all/0/1">D. J. McComas</a>, <a href="http://arxiv.org/find/physics/1/au:+Christian_E/0/1/0/all/0/1">E. R. Christian</a>, <a href="http://arxiv.org/find/physics/1/au:+Szalay_J/0/1/0/all/0/1">J. R. Szalay</a>, <a href="http://arxiv.org/find/physics/1/au:+Joyce_C/0/1/0/all/0/1">C. J. Joyce</a>, <a href="http://arxiv.org/find/physics/1/au:+Giacalone_J/0/1/0/all/0/1">J. Giacalone</a>, <a href="http://arxiv.org/find/physics/1/au:+Schwadron_N/0/1/0/all/0/1">N. A. Schwadron</a>, <a href="http://arxiv.org/find/physics/1/au:+Mitchell_D/0/1/0/all/0/1">D. G. Mitchell</a>, <a href="http://arxiv.org/find/physics/1/au:+Hill_M/0/1/0/all/0/1">M. E. Hill</a>, <a href="http://arxiv.org/find/physics/1/au:+Wiedenbeck_M/0/1/0/all/0/1">M. E. Wiedenbeck</a>, <a href="http://arxiv.org/find/physics/1/au:+McNutt_R/0/1/0/all/0/1">R. L. McNutt Jr.</a>, <a href="http://arxiv.org/find/physics/1/au:+Desai_M/0/1/0/all/0/1">M. I. Desai</a>, <a href="http://arxiv.org/find/physics/1/au:+Bale_S/0/1/0/all/0/1">Stuart D. Bale</a>, <a href="http://arxiv.org/find/physics/1/au:+Bonnell_J/0/1/0/all/0/1">J. W. Bonnell</a>, <a href="http://arxiv.org/find/physics/1/au:+Wit_T/0/1/0/all/0/1">Thierry Dudok de Wit</a>, <a href="http://arxiv.org/find/physics/1/au:+Goetz_K/0/1/0/all/0/1">Keith Goetz</a>, <a href="http://arxiv.org/find/physics/1/au:+Harvey_P/0/1/0/all/0/1">Peter R. Harvey</a>, <a href="http://arxiv.org/find/physics/1/au:+MacDowall_R/0/1/0/all/0/1">Robert J. MacDowall</a>, <a href="http://arxiv.org/find/physics/1/au:+Malaspina_D/0/1/0/all/0/1">David M. Malaspina</a>, <a href="http://arxiv.org/find/physics/1/au:+Pulupa_M/0/1/0/all/0/1">Marc Pulupa</a>, <a href="http://arxiv.org/find/physics/1/au:+Velli_M/0/1/0/all/0/1">M. Velli</a>, <a href="http://arxiv.org/find/physics/1/au:+Kasper_J/0/1/0/all/0/1">J.C. Kasper</a>, <a href="http://arxiv.org/find/physics/1/au:+Korreck_K/0/1/0/all/0/1">K.E. Korreck</a>, <a href="http://arxiv.org/find/physics/1/au:+Stevens_M/0/1/0/all/0/1">M. Stevens</a>, <a href="http://arxiv.org/find/physics/1/au:+Case_A/0/1/0/all/0/1">A.W. Case</a>, <a href="http://arxiv.org/find/physics/1/au:+Raouafi_N/0/1/0/all/0/1">N. Raouafi</a>

Observations at 1 au have confirmed that enhancements in measured energetic
particle fluxes are statistically 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 magnetic flux 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 isois
instruments during the first solar encounter. The distribution 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 isois
observations show a power-law distribution of waiting times, indicating a
correlated (non-Poisson) distribution. Analysis of low-energy isois data
suggests that the results are consistent with the 1 au studies, although we
find hints of some unexpected behavior. 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.

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