HR: 0800h
AN: P41B-01    [Abstracts]
TI: Ray Tracing Jupiter`s HOM Radio Emission
AU: Higgins, C
EM: chiggins@mtsu.edu
AF: Middle Tennessee State University, Dept. of Physics & Astronomy Box 71, 1301 E. Main St., Murfreesboro, TN 37132, United States
AU: * West, C
EM: carydaniel@gmail.com
AF: Middle Tennessee State University, Dept. of Physics & Astronomy Box 71, 1301 E. Main St., Murfreesboro, TN 37132, United States
AB: Cassini, Galileo, and Voyager spacecraft observations show well-defined attenuation features in the hectometer (HOM) spectrum of Jupiter's radio emission. The features are best displayed as frequency versus time spectrograms of HOM intensity between 500 - 3000 kHz. The bands have been shown by Gurnett et al. (1998) to be the result of propagation processes involving these emissions from opposite hemispheres. Enhancements in the HOM intensity and occurrence are seen along the edges of the observed attenuation features which may indicate caustic surfaces due to refraction along the propagation path. Using magnetic field and density models of the Jovian magnetosphere, we present some ray tracing analyses to show that radio wave refraction from density enhancements in the Io flux tube can produce the attenuation structures seen in the observations. This can provide boundaries to the electron density within the Io flux tube.
DE: 2756 Planetary magnetospheres (5443, 5737, 6033)
DE: 6939 Magnetospheric physics (2700)
DE: 6964 Radio wave propagation
SC: Planetary Sciences [P]
MN: 2007 Joint Assembly