Degree-1 magnetic excitation spectra for icy moons
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Matlab .mat files each containing a struct named FTdata with the fields below, containing information about the spatially uniform (degree-1) magnetic oscillations applied to each moon by their parent planet as a function of frequency. Used for determining the strength of induced magnetic fields from the moons from an interior conductivity structure. This dataset is compatible for use with the <em>PlanetProfile</em> framework for calculating the strength of induced magnetic field based in bulk properties of a moon in question. Save the files into the MagneticInduction/FieldData directory. Each .mat file contains a Matlab struct FTdata with the following fields: <strong>frequency</strong> - the excitation frequency at which oscillations occur in Hz. This is the independent variable for the other fields. <strong>Bx_fft</strong> - magnitude of the excitation field <em>B<sub>x</sub></em> component at each frequency of oscillation in nT. <strong>By_fft</strong> - magnitude of the excitation field <em>B<sub>y</sub></em> component at each frequency of oscillation in nT. <strong>Bz_fft</strong> - magnitude of the excitation field <em>B<sub>z</sub></em> component at each frequency of oscillation in nT. All vector components are in IAU coordinates, such that at the body center, +<em>x</em> is directed toward the parent planet, +<em>z</em> is directed along the body spin axis, and +<em>y</em> is directed approximately opposite to the orbital velocity to complete the right-handed set. Excitation fields are determined by evaluation of SPICE kernels over a years-long time series at the location of the body center. Position information is inserted into a magnetospheric model for the parent planet and a Fourier transform is calculated from the time series. These data are the results of the Fourier transform. The magnetic field models we use for each planet are: <strong>Jupiter</strong> - JRM09 + Connerney current sheet model (Connerney et al., 2018, 1981) <strong>Saturn</strong> - The model of Burton et al. (2010) <strong>Uranus</strong> - AH<sub>5</sub> model (Herbert, 2009) <strong>Neptune</strong> - The model of Connerney et al. (1991)
