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Differential rotation of the magnetic fields of gaseous planets
Author(s) -
Dessler A. J.
Publication year - 1985
Publication title -
geophysical research letters
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.007
H-Index - 273
eISSN - 1944-8007
pISSN - 0094-8276
DOI - 10.1029/gl012i005p00299
Subject(s) - differential rotation , uranus , physics , planet , dynamo , rotation period , dynamo theory , jupiter (rocket family) , latitude , dipole model of the earth's magnetic field , magnetic dipole , mercury's magnetic field , neptune , magnetic field , saturn , jovian , magnetosphere , geophysics , astronomy , earth's magnetic field , l shell , interplanetary magnetic field , solar wind , stars , space shuttle , quantum mechanics
We argue that, with regard to the spin rate of magnetic field structure as a function of latitude, the behavior of the magnetic fields of gaseous planets is more analogous to the Sun than the Earth. Certain Jovian magnetospheric phenomena differ in repetition period by 3%. In order to explain Jupiter's two distinct periodicities, it is hypothesized that the spin period of the planet's magnetic features is a function of both latitude and the size of the feature, with smaller high‐latitude features rotating slower than either low‐latitude features or the dominant dipole moment. Similarly, the low‐latitude planetary spin period of Saturn is shorter than the presently accepted single value because the present value is based on a high‐latitude magnetic phenomenon. We should also expect differential rotation of surface magnetic features at both Uranus and Neptune if they prove to have internal dynamo‐generated magnetic fields.