Plasma electrons in Saturnʹs magnetotail: Structure, distribution and energisation

In this paper Saturnʹs nightside and pre-dawn electron (0.5 eV–28 keV) plasma sheet is studied using Cassini plasma electron and magnetic field data from 2006. Case studies are presented which exemplify the typical and atypical states of the plasma sheet, and are complemented by a statistical study of the plasma sheet. It will be shown that Saturnʹs nightside and pre-dawn electron plasma sheet exists in two states: a quiescent state with a steady electron temperature of ∼ 100 eV and where the electron distribution functions are best characterised by Kappa distributions, and a disturbed state where the electrons are hot ( ∼ 1 keV ) and often seen in alternating layers between warm and hot populations. Evidence is also presented for bimodal cold/warm (both quiet and disturbed states) and warm/hot distributions (disturbed states). The disturbed states are qualitatively similar to electron distributions from Earthʹs magnetotail during intervals of reconnection and we argue that these disturbed states also result from periods of tail reconnection. We present statistics of electron number density, temperature, partial electron beta, and pressure, and show that large values of partial beta are necessary but not sufficient to uniquely identify the central plasma sheet. Finally the thermodynamic properties of the electron plasma sheet are studied and we show that the electrons behave isothermally. These results are important for modelling and theoretical analyses, and for use in studies which examine dynamics in Saturnʹs magnetosphere.