Other
Scientific paper
May 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agusmsm44a..04w&link_type=abstract
American Geophysical Union, Spring Meeting 2004, abstract #SM44A-04
Other
2753 Numerical Modeling, 2784 Solar Wind/Magnetosphere Interactions, 5737 Magnetospheres (2756), 6220 Jupiter
Scientific paper
It has long been recognized that the solar wind and its interplanetary magnetic field (IMF) drive magnetospheric dynamics at the Earth. Jupiter`s magnetosphere on the other hand is dominated by a massive rotating equatorial plasma sheet and the solar wind and the IMF are not thought be as important as at Earth. We have carried out global MHD simulations of the response of the magnetospheres of the Earth and Jupiter to northward and southward turnings of the IMF. The most dramatic changes occurred when the IMF at the Earth was southward and that at Jupiter was northward. (Jupiter`s intrinsic magnetic field is in the opposite direction to that of the Earth.) In all cases the IMF was turned southward or northward and held constant. For southward IMF at the Earth dayside reconnection was followed by reconnection in the near-Earth magnetotail and a plasmoid was launched tailward. A steadily reconnecting system with a neutral line at x=-16RE then evolved which lasted for the duration of the numerical experiment. In similar fashion dayside reconnection was followed by tail reconnection at Jupiter. However, unlike the case at Earth, the reconnection at Jupiter was episodic both on the dayside and in the tail. Following the onset of dayside reconnection large amplitude waves that modulated the reconnection formed on the Jovian magnetopause. The waves had a wavelength of approximately 30RJ and a period of about 30 hours. During each episode in the tail a near-Jupiter (x<-100RJ) neutral line and plasmoid formed. Then both the neutral line and the plasmoid moved tailward and the process started again about 30 hours later.
Fukazawa Kenji
Ogino Takeshi
Walker Ray J.
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