Abstract
An axisymmetric octupole model of Saturn's planetary magnetic field is proposed here. This three parameter model, characterized by the Schmidt-normalized spherical harmonic coefficients g01 = 21,535 nT, g02 = 1,642 nT and g03 = 2,743 nT, is extremely efficient in representing the main magnetic field of Saturn and reconciling the in situ magnetic field observations obtained by Pioneer 11 with those obtained by the Voyager 1 and 2 spacecraft. Saturn's unique magnetic field configuration is thus not that of a simple displaced dipole but rather appears to be the axisymmetric part of a complex dynamo field. This result is consistent with Stevenson's model of the interior of Saturn1, in which the differential rotation of a metallic fluid shell above the active dynamo region attenuates all non-axisymmetric components of the dynamo field.
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Connerney, J., Ness, N. & Acuña, M. Zonal harmonic model of Saturn's magnetic field from Voyager 1 and 2 observations. Nature 298, 44–46 (1982). https://doi.org/10.1038/298044a0
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DOI: https://doi.org/10.1038/298044a0
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