HR: 09:15h
AN: SM41B-06 [Abstracts]
TI: Interaction of Interplanetary Shocks with the Earth's Magnetosphere: Observations and Global
MHD Simulations Compared During the Nov 9, 2002 Event
AU: Andreeova, K
EM: andreeova@seznam.cz
AF: Charles University Prague, V Holesovickach 2, Prague, CZ-18000, Czech Republic
AU: * Pulkkinen, T I
EM: tuija.Pulkkinen@fmi.fi
AF: Finnish Meteorological Institute, POBox 503, Helsinki, FI-00101, Finland
AU: Laitinen, T V
EM: tiera.laitinen@fmi.fi
AF: Finnish Meteorological Institute, POBox 503, Helsinki, FI-00101, Finland
AU: Prech, L
EM: lubomir.prech@mff.cuni.cz
AF: Charles University Prague, V Holesovickach 2, Prague, CZ-18000, Czech Republic
AB:
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.
DE: 2139 Interplanetary shocks
DE: 2752 MHD waves and instabilities (2149, 6050, 7836)
DE: 2753 Numerical modeling
DE: 2784 Solar wind/magnetosphere interactions
SC: SPA-Magnetospheric Physics [SM]
MN: 2007 Fall Meeting