Authors: Alicia Petersen (University of Florida), David Galarza (University of Florida)

Recent Parker Solar Probe (PSP) observations nearer the Sun than ever before likely contains key information about properties of the heliospheric magnetic field (HMF) throughout the inner heliosphere between active regions on the solar surface and the wealth of historical in situ observations we have had nearer the Earth, including observations by the Advanced Composition Explorer (ACE) and WIND at the L1 Lagrange point.

Suprathermal electrons (SEs) are particularly interesting for studying the topological properties and potential histories of the heliospheric magnetic field lines that they propagate along. Classifying solar wind observations by the pitch angle distributions of suprathermal electrons yield key differences due to variations in the HMF and plasma properties within the inner heliosphere responsible for SE scattering. Identifying which properties of the HMF result in which SE pitch angle distributions, is non-trivial. Thus modeling the resulting pitch angle distributions of SEs given an initial HMF, may produce the array of signatures needed to identify key features of the HMF from observations of suprathermal electrons. If suprathermal electrons observed in situ can be used to identify properties of the HMF lines they have traversed, then new avenues for connecting transient events to their origins become available.