Modeling Jovian Synchrotron Radiation
Comparison between 21cm VLA maps (left) and the JPL model (right) at CML=120o (top) and 200o (bottom).
We have a collaborative research effort between my group at UCLA, the radio physics group at JPL, (S. Levin, S. Gulkis) and the Salammbo modeling effort at SWRI (S. Bolton, D.Santos-Costa) to understand the physical processes responsible for synchrotron emission from relativistic electrons in the Jovian inner magnetosphere. The study involves the use of radio emission data from single dish antennae, the Very Large Array and most recently from the Cassini spacecraft, together with theoretical modeling of key physical processes.
Santos-Costa, D. S., S. Bolton, R. M. Thorne,
Y. Miyoshi., and
Bolton, S. J., R. M. Thorne, S. Bourdarie, B. H. Mauk, and I. de Pater (2004), Jupiterís inner radiation belts, in Jupiter: The Planet, Satellites, and
Magnetosphere, edited by F. Bagenal, T. Dowling,
Bolton, S. J., M. Jansen, R. M. Thorne, S. Levin, M. Klein, S. Gulkis, T. Bastian, R. Sault, C. Elachi, M. Hofstadter, A. Bunker, G. Dulk, E. Gudim, M. Hamilton, W. Johnson, Y. Leblanc, O. Liepack, R. McLeod, J. Roller, L. Roth, and R. West. Cassini and ground-based observations of synchrotron emission from Jupiterís radiation belts, Nature, 415, 987, 2002.
Levin, S. M., S. J. Bolton, S. L. Gulkis, M. J. Kline, B. Bhattacharya, and R. M. Thorne, Modeling Jupiterís synchrotron radiation, Geophys. Res Lett., 28, 903-906, 2001.