Supercorotating return flow from reconnection in Saturn's magnetotail

Details Supercorotating return flow from reconnection in Saturn's magnetotail Supercorotating return flow from reconnection in Saturn's magnetotail

Feb 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011georl..3803103m&link_type=abstract

Geophysical Research Letters, Volume 38, Issue 3, CiteID L03103

Physics

Magnetospheric Physics: Planetary Magnetospheres (5443, 5737, 6033), Magnetospheric Physics: Magnetospheric Configuration And Dynamics, Magnetospheric Physics: Magnetic Reconnection (7526, 7835), Planetary Sciences: Solar System Objects: Saturn, Magnetospheric Physics: Solar Wind/Magnetosphere Interactions

Scientific paper

Detecting plasma dynamics in Saturn's magnetosphere is essential for understanding energy flow through the system. It has been proposed that both the Dungey and Vasyliunas cycles operate at Saturn, and the competition between these cycles has been debated. We examine data taken by the Cassini spacecraft in Saturn's post-dawn magnetosphere, ˜17.5 Saturn radii from the planet, and identify an example of return flow from magnetotail reconnection. The flow included water group ions and had elevated ion temperatures (of order 1 keV), consistent with Vasyliunas cycle return flow. The flow was also supercorotating (˜200 km s-1, ˜120% of corotation), which is highly atypical of Saturn's outer magnetosphere. Our results suggest that return flows are time-variable, and our results concerning Dungey cycle return flows are inconclusive. We propose that supercorotating flows in Saturn's dawn magnetosphere strongly influence the current system that is responsible for the planet's main auroral emission.

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