Physics
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsm41b..06a&link_type=abstract
American Geophysical Union, Fall Meeting 2007, abstract #SM41B-06
Physics
2139 Interplanetary Shocks, 2752 Mhd Waves And Instabilities (2149, 6050, 7836), 2753 Numerical Modeling, 2784 Solar Wind/Magnetosphere Interactions
Scientific paper
It is widely known that interplanetary shocks cause pressure pulses and launch a variety of waves into the magnetosphere. Our analysis of several interplanetary shocks reveals that the disturbance speeds are higher in the magnetosphere than in the solar wind and gradually increase from the dayside to the nightside magnetotail. On November 9th, 2002, observations of two consecutive fast forward interplanetary shocks were provided by several widely separated satellites: ACE, Wind, Genesis, SOHO, and Geotail in the solar wind, GOES series spacecraft, Polar, and Cluster in the magnetosphere. In addition, the shock propoagation was monitored by networks of ground magnetometers. This rich set of multipoint observations allows us to monitor in detail the propagation of the disturbance from the solar wind to the near-Earth's magnetosphere. In order to resolve causes for the unusual double onset structures observed at geostationary orbit and to verify our disturbance speed estimations, we have used the GUMICS-4 global MHD code to simulate the entire sequence of events. The simulation gives us a global picture of the shock -- magnetosphere interaction, which allows us to match many features with the satellite observations and helps to interpret to satellite measurements in different parts of the magnetosphere. We demonstrate the capabilities and discuss the constraints of the simulation model to describe such rapidly propagating dynamic events.
Andréeová Katerina
Laitinen T. V.
Prech Lubomír
Pulkkinen Tuija I.
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