Solar wind and rotational effects on the 3d configuration of Saturn's magnetosphere: Observations, theory, and modelling, in the Cassini era

Details Solar wind and rotational effects on the 3d configuration of Saturn's magnetosphere: Observations, theory, and modelling, in the Cassini era Solar wind and rotational effects on the 3d configuration of Saturn's magnetosphere: Observations, theory, and modelling, in the Cassini era

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsm52a..01a&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SM52A-01

Physics

2706 Cusp, 2740 Magnetospheric Configuration And Dynamics, 2784 Solar Wind/Magnetosphere Interactions, 5737 Magnetospheres (2756), 6275 Saturn

Scientific paper

Cassini has now provided over 50 orbits of high quality data and is revolutionising our understanding of Saturn's magnetosphere. The post-Voyager view was of a magnetosphere somewhat intermediate between the terrestrial and jovian magnetospheres. Cassini observations, and recent modelling and theoretical work, are showing us that the distinction is not so straightforward. Saturn's&pmagnetosphere appears to be unique in the solar system in that the solar wind and rotational effects strongly interact to produce a highly complex magnetosphere. For example, observations have shown (Arridge et al., 2007a) that the magnetodisc is suppressed on the dayside when the magnetosphere is in a compressed state showing that the effect of rotation on the magnetic field (Arridge et al., 2007b; Bunce et al. 2007) can be significantly altered by the solar wind in a highly time-dependent manner. In this talk we discuss the roles of solar wind and rotational forcing in producing the complex three-dimensional kronian magnetosphere. In particular we discuss: the compressibility of the magnetosphere, observations of the polar cusp and evidence for an open magnetosphere, formation of the magnetotail, morphology of the plasma sheet, and magnetodisc models.

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