Physics
Scientific paper
Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsm11a1573i&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #SM11A-1573
Physics
2736 Magnetosphere/Ionosphere Interactions (2431), 2764 Plasma Sheet, 2778 Ring Current, 2784 Solar Wind/Magnetosphere Interactions, 2788 Magnetic Storms And Substorms (7954)
Scientific paper
This study investigates the role of fluctuations in the solar wind parameters in triggering a magnetic storm and assesses the storm simulation ability of Space Weather Modeling Framework (SWMF) through model- data comparison. The event of September 22, 1999 is examined through global magnetosphere simulations, using as input ACE observations (16 sec temporal resolution) along with running averages of this data with windows of 4, 60, 120 and 180 minutes. It is noted that averaged solar wind input produces a double dip, fast recovery phase with a shorter main phase compared with the 16 second resolution input. Also, smoothing the input with a window larger than 60 minutes changes the entire magnetosphere and reduces the plasma sheet density/pressure, therefore a less intense storm develops. Is is worth to mention that the main phase for this magnetic storm lasted 3 hours, while the rapid drop in Dst index took less than one hour. This explains the change in the Dst profile for the 120 and 180 minutes averaged input. Also, comparison with the Dst predictions (O'Brien and McPherron, 2000) are presented and discussed. For all cases studied, there are no significant differences for Cross Polar Cap Potential (CPCP) in both hemispheres, while midnight plasma sheet density shows a sharp drop when the input is averaged over 4 minutes or more. Moreover, 4 minutes and 60 minutes temporal resolution inputs produce a larger disturbance than the 16 seconds resolution solar wind input.
Ilie Raluca
Liemohn Michael W.
Ridley A. A.
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