Plasma-depleted flux tubes in the Saturnian magnetosphere and their implications

Details Plasma-depleted flux tubes in the Saturnian magnetosphere and their implications Plasma-depleted flux tubes in the Saturnian magnetosphere and their implications

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsm11a1997p&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SM11A-1997

Physics

[5737] Planetary Sciences: Fluid Planets / Magnetospheres

Scientific paper

The Saturnian magnetosphere is driven internally by the acceleration of plasma originating from moon, Enceladus, which adds hundreds of kilograms of water group neutrals and plasma every second. The newly added plasma is accelerated to the rotational speed of the planet and convects outwards from the inner magnetosphere. Eventually it is lost through magnetic reconnection in the tail, resulting in massive plasmoids moving tailward and "empty" flux tubes moving Saturnward. These plasma-depleted flux tubes return magnetic flux from the tail back to the inner magnetosphere, due to interchange instability in a centrifugally driven system. We examine the Cassini magnetometer data and CAPS data to understand the properties of such flux tubes and their statistical behavior. The occurrence of these plasma-depleted flux tubes also gives us information on how the magnetospheric dynamics are affected by mass transport. We examine whether the occurrence rate is ordered by local time and whether it is correlated with the phase of Enceladus.

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