AN INTERCOMPARISON OF 3-DIMENSIONAL RECONSTRUCTION TECHNIQUES USING DATA AND MODELS OF JUPITERS SYNCHROTRON-RADIATION

We present and compare results from two different tomographic reconstr uction techniques: a backprojection technique [from de Pater er al., 1 997b] and a three-dimensional (3-D) Fourier technique [from Sault er a l,, 1997]. We applied both techniques to very large array (VLA) data o f Jupiter's synchrotron radiation and to models which simulate 2-D ima ges of Jupiter's radio emission [from de Pater ef al., 1997a]. The 3-D images thus constructed represent the apparent radio emissivity. Resu lts from the two techniques are quite compatible. A comparison between the tomographic reconstructions of the data and model yields informat ion on models of the electron flux, j(L, alpha(e), E), and the magneti c held configuration. At first glance, results from the data and model agree quite well. Longitudinal differences between the data and model suggest the need for modifications to the magnetic field model, while differences in the radial profile are caused by imperfections in the radial profile of the electron flux. We suggest that the magnetic equa torial surface should be less warped than in the O6 model. We further find that the change in the modeled pitch angle distribution at Amalth ea's orbit [from de Pater et al., 1997a] should be modified by, for ex ample, the inclusion of diffusion both in pitch angle and L, while the re also appear to be more emitters at high latitudes outside of Amalth ea's orbit than assumed in the model.