Session: Heliophysics and the Solar System
Name: Ms. Alexandra Triantopoulou (National & Kapodistrian Univ. of Athens)
Coauthors:
Nasi Afroditi (NKUA, Greece)
Katsavrias Christos (NKUA, Greece)
Sandberg Ingmar (SPARC & Aerospace Science and Technology, NKUA, Greece)
Daglis Ioannis A. (NKUA, Greece & Hellenic Space Center, Greece)
Type: Poster
Title: Impact of high-speed solar wind streams on the dynamic variations of the electron population in the outer Van Allen belt
Abstract:
More than half a century after the discovery of Van Allen radiation belts, their
dynamics are still not fully understood. The variability of the outer radiation belt
electrons is related to geospace disturbances due to the interaction of solar wind with
the terrestrial magnetosphere. The relativistic and ultra-relativistic electron population
can be enhanced or depleted depending on the balance of the various acceleration and
loss mechanisms. This variability depends significantly on the solar wind driver type.
One of the most common solar wind drivers that affect, amongst others, the electrons
of the outer radiation belt is the High-Speed Streams (HSSs) following Stream
Interaction Regions (SIRs). Their effect on the various energetic electron populations
is a major theme of space research.
In this work, we examine the electron phase space density (PSD) during 30 SIRdriven events that occurred during the RBSP era (2012-2018), in terms of superposed
epoch analysis (SEA), for seed, relativistic and ultra-relativistic electrons (μ=100, 1000,
5000 MeV/G). Furthermore, we examine three distinct values of the second adiabatic
invariant (K=0.03, 0.09, 0.15 G1/2RE) in order to compare the differences between local
acceleration and radial diffusion. In addition, we selected the time of maximum solar
wind pressure (Pswmax) as the zero epoch time for all events, with the aim of extracting
a statistical study, through time and radial profiles, of the response of the outer belt
electron population on this solar wind driver