Properties of the magnetic field and plasma in the kronian magnetotail lobes and current sheet

Details Properties of the magnetic field and plasma in the kronian magnetotail lobes and current sheet Properties of the magnetic field and plasma in the kronian magnetotail lobes and current sheet

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufm.p33b1285j&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #P33B-1285

Physics

[2744] Magnetospheric Physics / Magnetotail, [2764] Magnetospheric Physics / Plasma Sheet, [2784] Magnetospheric Physics / Solar Wind/Magnetosphere Interactions

Scientific paper

Knowledge of the properties of the magnetotail lobes is important for understanding the structure, equilibrium and dynamics of the magnetotail and magnetosphere as a whole. In this presentation we use Cassini magnetometer and electron spectrometer data to characterize the magnetic field in Saturn’s magnetotail lobes throughout the nominal mission, with particular emphasis on the deep tail orbits out to ~65 RS in 2006. We compare the magnetic pressure in the central plasma sheet with that in the lobes to estimate plasma pressures in the plasma sheet and study the radial, local time and longitudinal profiles of lobe magnetic field strength and pressure. Power-law fits for the magnetic field strength and pressure as a function of radial distance are presented, with a field strength falloff of R-1.11. Estimates of the lobe plasma density are used to estimate the Alfvén speed. The effects of hinging of the current sheet on the nightside are observed and their relationship to solar wind conditions explored. Lobe conditions during “quiet” periods are compared and contrasted with disturbed periods where travelling compression regions and other such structures are observed. By comparing the average fitted lobe field strength with observations in the magnetotail, we attempt to investigate the typical length of the “growth phase” of substorm-like events at Saturn, and to quantify the amount of open flux closed during such events. Lastly, we discuss our results in the context of the Earth and Jupiter.

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