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Ganymede MHD Model: Magnetospheric Context for Juno’s PJ34 Flyby
  • +8
  • Stefan Duling,
  • Joachim Saur,
  • George Clark,
  • Frederic Allegrini,
  • Thomas K. Greathouse,
  • Randy Gladstone,
  • William S Kurth,
  • John E. P. Connerney,
  • Fran Bagenal,
  • Ali H. Sulaiman,
  • Ali H. Sulaiman
Stefan Duling
University of Cologne, University of Cologne, University of Cologne

Corresponding Author:[email protected]

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Joachim Saur
University of Cologne, University of Cologne, University of Cologne
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George Clark
Johns Hopkins University Applied Physics Laboratory, Johns Hopkins University Applied Physics Laboratory, Johns Hopkins University Applied Physics Laboratory
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Frederic Allegrini
Southwest Research Institute, Southwest Research Institute, Southwest Research Institute
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Thomas K. Greathouse
SWRI, SWRI, SWRI
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Randy Gladstone
Southwest Research Institute, Southwest Research Institute, Southwest Research Institute
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William S Kurth
University of Iowa, University of Iowa, University of Iowa
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John E. P. Connerney
NASA Goddard Space Flight Center, NASA Goddard Space Flight Center, NASA Goddard Space Flight Center
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Fran Bagenal
University of Colorado Boulder, University of Colorado Boulder, University of Colorado Boulder
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Ali H. Sulaiman
University of Iowa
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Ali H. Sulaiman
University of Minnesota, University of Minnesota
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Abstract

On June 7th, 2021 the Juno spacecraft visited Ganymede and provided the first in situ observations since Galileo’s last flyby in 2000. The measurements obtained along a one-dimensional trajectory can be brought into global context with the help of three-dimensional magnetospheric models. Here we apply the magnetohydrodynamic model of Duling et al. (2014) to conditions during the Juno flyby. In addition to the global distribution of plasma variables we provide mapping of Juno’s position along magnetic field lines, Juno’s distance from closed field lines and detailed information about the magnetic field’s topology. We find that Juno did not enter the closed field line region and that the boundary between open and closed field lines on the surface matches the poleward edges of the observed auroral ovals. To estimate the sensitivity of the model results, we carry out a parameter study with different upstream plasma conditions and other model parameters.