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Geophysical Research Letters

Volume 32, Issue 20
Space Sciences
Free Access

Global MHD simulations of Saturn's magnetosphere at the time of Cassini approach

K. C. Hansen

E-mail address:kenhan@umich.edu

Department of Atmospheric, Oceanic and Space Science, University of Michigan, Ann Arbor, Michigan, USA

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A. J. Ridley

Department of Atmospheric, Oceanic and Space Science, University of Michigan, Ann Arbor, Michigan, USA

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G. B. Hospodarsky

Department of Physics and Astronomy, University of Iowa, Iowa City, Iowa, USA

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N. Achilleos

Space and Atmospheric Physics, Imperial College, London, UK

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M. K. Dougherty

Space and Atmospheric Physics, Imperial College, London, UK

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T. I. Gombosi

Department of Atmospheric, Oceanic and Space Science, University of Michigan, Ann Arbor, Michigan, USA

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G. Tóth

Department of Atmospheric, Oceanic and Space Science, University of Michigan, Ann Arbor, Michigan, USA

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First published: 19 July 2005
https://doi.org/10.1029/2005GL022835
Cited by: 47

Abstract

[1] We present the results of a 3D global magnetohydrodynamic simulation of the magnetosphere of Saturn for the period of Cassini's initial approach and entry into the magnetosphere. We compare calculated bow shock and magnetopause locations with the Cassini measurements. In order to match the measured locations we use a substantial mass source due to the icy satellites (∼1 × 1028 s−1 of water product ions). We find that the location of bow shock and magnetopause crossings are consistent with previous spacecraft measurements, although Cassini encountered the surfaces further from Saturn than the previously determined average location. In addition, we find that the shape of the model bow shock and magnetopause have smaller flaring angles than previous models and are asymmetric dawn‐to‐dusk. Finally, we find that tilt of Saturn's dipole and rotation axes results in asymmetries in the bow shock and magnetopause and in the magnetotail being hinged near Titan's orbit (∼20 RS).

Number of times cited: 47

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