Abstract
The existence of a magnetic field associated with Jupiter was first postulated by radio- astronomers to explain the observed characteristics of Jovian non-thermal radio emissions at decimetric and decametric wave-lengths. It is now clearly established that synchrotron radiation by relativistic electrons trapped in the strong planetary field is responsible for the decimetric emissions. On the other hand the situation at decametric wavelengths is substantially more complex since the sources and physical processes responsible for this radiation have yet to be identified (see reviews by Warwick, 1967; Carr and Gulkis, 1969). A complete understanding of the physics of the Jovian magnetosphere requires a detailed knowledge of the strength and geometry of the planetary magnetic field. In this paper we review our current knowledge of Jupiter’s magnetic field and its implications for the study of trapped particle populations and planetary radio emissions. We shall be concerned primarily with the intrinsic planetary field which dominates the inner magneto- sphere up to a distance of 10 to 12 Jovian radii where other phenomena, such as ring currents and diamagnetic effects of trapped charged particles, become significant (Van Allen et al, 1974; Smith et al., 1974).KeywordsRadiation BeltMagnetic Field ModelFluxgate MagnetometerTilted DipoleJovian MagnetosphereThese keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.
Published Version
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call