Suprathermal electron loss cone distributions in the solar wind: ULYSSES observations

Details Suprathermal electron loss cone distributions in the solar wind: ULYSSES observations Suprathermal electron loss cone distributions in the solar wind: ULYSSES observations

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995sowi.conf...74p&link_type=abstract

Los Alamos National Lab., International Solar Wind 8 Conference, p. 74

Computer Science

Electron Beams, Electron Distribution, Solar Electrons, Solar Wind, Hot Electrons, Heat Flux, Stellar Mass Ejection, Ulysses Mission, Shock Waves, Interplanetary Magnetic Fields

Scientific paper

Solar wind suprathermal electron distributions in the solar wind generally carry a field-aligned antisunward heat flux. Within coronal mass ejections and upstream of strong shocks driven by corotating interaction regions (CIRs), counterstreaming electron beams are observed. We present observations by the Ulysses solar wind plasma experiment of a new class of suprathermal electron signatures. At low solar latitudes and heliocentric distances beyond 3.5 AU Ulysses encountered several intervals, ranging in duration from 1 hour to 22 hours, in which the suprathermal distributions included an antisunward field-aligned beam and a return population with a flux dropout typically spanning +/- 60 deg from the sunward field-aligned direction. All events occurred within CIRs, downstream of the forward and reverse shocks or waves bounding the interaction regions. We evaluate the hypothesis that the sunward-moving electrons result from reflection of the antisunward beams at magnetic field compressions downstream from the observations, with wide loss cones caused by the relatively weak compression ratio. This hypothesis requires that field magnitude within the CIRs actually increase with increasing field-aligned distance from the Sun. Details of the electron distributions and ramifications for CIR and shock geometry will be presented.

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