HR: 0800h
AN: SH51B-1204    [Abstracts]
TI: Interaction of Interplanetary Shocks With the Earth's Foreshock
AU: * Prech, L
EM: lubomir.prech@mff.cuni.cz
AF: Charles University Prague, Faculty of Mathematics and Physics, V Holesovickach 2, Prague, 18000 Czech Republic
AU: Andreeova, K
EM: katerina.andreeova@mff.cuni.cz
AF: Charles University Prague, Faculty of Mathematics and Physics, V Holesovickach 2, Prague, 18000 Czech Republic
AU: Koval, A
EM: koviand@yahoo.com
AF: Charles University Prague, Faculty of Mathematics and Physics, V Holesovickach 2, Prague, 18000 Czech Republic
AU: Safrankova, J
EM: jana.safrankova@mff.cuni.cz
AF: Charles University Prague, Faculty of Mathematics and Physics, V Holesovickach 2, Prague, 18000 Czech Republic
AU: Nemecek, Z
EM: zdenek.nemecek@mff.cuni.cz
AF: Charles University Prague, Faculty of Mathematics and Physics, V Holesovickach 2, Prague, 18000 Czech Republic
AU: Kasper, J C
EM: jck@mit.edu
AF: MIT, Kavli Institute for Astrophysics and Space Research, 77 Massachusetts Avenue, Cambridge, MA 02139 United States
AB: Interplanetary shocks have been often reported in the solar wind near the Earth, many of them were observed by several spacecraft on their path from L1 to the Earth's magnetosphere. The study of their gradual evolution belongs to important topics of the Sun--Earth's system investigations. Foreshock is a complex region upstream of the Earth's bow shock where solar wind plasma becomes affected by the presence of the Earth's magnetoshere. In our contribution, we discuss simultaneous observations of interplanetary shocks in different parts of the Earth's foreshock and compare their properties to those determined from data obtained in the solar wind outside of the foreshock, near L1 and/or in the magnetosheath. While many interplanetary shocks retain most of their signatures along their path toward the Earth, particular observations show that some shock discontinuities can change their properties, for example they disperse their fronts into slow interplanetary magnetic field rotations. As these cases were often located inside the Earth's foreshock, a question arises about a significance of the foreshock in these processes. We attempt to describe conditions that lead to the strongest foreshock alterations and substantial modifications of the interplanetary shock itself.
DE: 2139 Interplanetary shocks
DE: 2154 Planetary bow shocks
DE: 2784 Solar wind/magnetosphere interactions
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005