Magnetic field disturbances in the Jovian magnetosphere due to large dynamic pressure enhancements in the solar wind

Details Magnetic field disturbances in the Jovian magnetosphere due to large dynamic pressure enhancements in the solar wind Magnetic field disturbances in the Jovian magnetosphere due to large dynamic pressure enhancements in the solar wind

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsm33a1252t&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #SM33A-1252

Physics

7843 Numerical Simulation Studies, 5737 Magnetospheres (2756), 2740 Magnetospheric Configuration And Dynamics, 2756 Planetary Magnetospheres (5443, 5737, 6030), 2784 Solar Wind/Magnetosphere Interactions

Scientific paper

In order to understand the Jovian magnetospheric response to large enhancements of solar wind dynamic pressure, we investigate magnetic field disturbances observed by the Galileo spacecraft located inside the Jovian magnetosphere. A lack of solar wind monitoring just outside the Jovian magnetosphere is complemented by performing one-dimensional magnetohydrodynamic (MHD) simulation. Solar wind data obtained from the Wind and ACE spacecraft in the vicinity of the Earth are used as input parameters of the solar wind simulation. A verification test of simulated solar wind parameters is performed by comparing them with actual solar wind parameters obtained by the Ulysses spacecraft in the vicinity of the Jovian orbit. The estimated error of shock arrival time is <2 days if the acute angle of Jupiter-Sun-Earth is <50º. We select 9 events that meet a criterion of event selection: an increase of solar wind dynamic pressure >0.3 nPa in a few hours at the Jovian orbit. Characteristic changes of magnetic field disturbances are found for all of the 9 events. For 8 of the 9 events, the rectangular waveform with the rotation period of about 10 hours becomes irregular in response to the large dynamic pressure change. Furthermore, it is found that the amplitude of the turbulent magnetic field in the ultra-low frequency (ULF) range of 0.3 - 10 mHz increases simultaneously with and/or after irregular waveform changes, in proportion to the maximum amplitude of solar wind dynamic pressure enhancements.

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