The role of Alfvénic turbulence in Jupiter's M-I coupling

Details The role of Alfvénic turbulence in Jupiter's M-I coupling The role of Alfvénic turbulence in Jupiter's M-I coupling

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsm22c..01s&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SM22C-01

Physics

2704 Auroral Phenomena (2407), 2736 Magnetosphere/Ionosphere Interactions, 2756 Planetary Magnetospheres (5443, 5737, 6030), 6220 Jupiter

Scientific paper

In our presentation we will discuss the role of Alfvén waves in Jupiter's M-I coupling and their connection to Jupiter's powerful auroral oval, with an emitted UV power about three orders of magnitude larger than Earth's aurora. We will relate the mechanisms in Jupiter's magnetosphere to understanding developed in the Earth context. One of the main differences between Jupiter's and the Earth's magnetosphere is the quasi steady source of Alfvén waves deep inside Jupiter's magnetosphere triggered by radial plasma transport. These Alfvénic fluctuations propagate along the closed field lines in Jupiter's middle magnetosphere and counter propagating waves interact non-linearly to create a turbulent cascade of small scale Alvénic fluctuations. When the scales of the fluctuations reach kinetic scales, the fluctuations are dissipated at high magnetic latitudes. At the presence of a net field-aligned electric current also due to radial mass transport, the dissipation process accelerates electrons to produce Jupiter's main auroral oval. We will discuss these mechanisms in detail. We will also present Galileo spacecraft measurement of the Poynting flux and spectral energy fluxes associated with the Alfvénic fluctuations and compare them with recent Hubble Space Telescope (HST) Observations of Jupiter's main auroral oval. We show that the voltage -- energy flux relationship inferred from latest HST observations (private communication J.-C. Gérard) fit well with our theoretical model predictions.

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