Modeling of Saturn kilometric radiation arcs and equatorial shadow zone

Details Modeling of Saturn kilometric radiation arcs and equatorial shadow zone Modeling of Saturn kilometric radiation arcs and equatorial shadow zone

Oct 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008jgra..11310213l&link_type=abstract

Journal of Geophysical Research, Volume 113, Issue A10, CiteID A10213

Physics

Plasma Physics

16

Planetary Sciences: Solar System Objects: Saturn, Solar Physics, Astrophysics, And Astronomy: Radio Emissions, Space Plasma Physics: Charged Particle Motion And Acceleration, Space Plasma Physics: Wave/Particle Interactions (2483, 6984)

Scientific paper

Accelerated electrons gyrating around Saturn's auroral (high latitude) magnetic field lines generate the intense Saturnian kilometric radiation (SKR). This radio emission is thought to be generated via the cyclotron maser instability (CMI) that predicts a strong anisotropy of the beaming pattern of the emission. Resulting visibility effects were suspected to be at the origin of characteristic features observed in Cassini's dynamic spectra as arc-shaped structures and shadow zones. By using the Planetary Radio Emissions Simulator (PRES) code, we model these visibility effects and their consequence on Cassini's observations of SKR: we compute the dynamic spectra resulting from the beaming pattern of CMI-generated SKR and its intersection with Cassini's trajectory. The SKR beaming pattern and its dependence on the frequency is computed for two typical electron distributions observed in auroral regions: a loss cone (favoring oblique emission) or a shell (favoring perpendicular emission). We successfully fit observed arc-shaped structures and shadow zones. Although oblique and perpendicular emissions both allow to produce radio arcs, the fit is better in the oblique case. Similarities and differences between observations and model results are discussed and perspectives are outlined.

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