HR: 1400h
AN: SM33B-08    [Abstracts]
TI: Interaction of Interplanetary Shocks With the Bow Shock and Their Propagation Within the Magnetosheath
AU: * Safrankova, J
EM: jana.safrankova@mff.cuni.cz
AF: Charles University, Faculty of Mathematics and Physics, V Holesovickach 2, Prague, 180 00, Czech Republic
AU: Nemecek, Z
EM: zdenek.nemecek@mff.cuni.cz
AF: Charles University, Faculty of Mathematics and Physics, V Holesovickach 2, Prague, 180 00, Czech Republic
AU: Prech, L
EM: lubomir.prech@mff.cuni.cz
AF: Charles University, Faculty of Mathematics and Physics, V Holesovickach 2, Prague, 180 00, Czech Republic
AU: Samsonov, A
EM: yasam00@yandex.ru
AF: St. Petersburg State University, St. Petersburg, St. Petersburg, Russian Federation
AU: Koval, A
EM: a.s.koval@gmail.com
AF: NASA GSFC, Greenbelt, Greenbelt, MA MD 20771, United States
AU: Andreeova, K
EM: Andreeova@seznam.cz
AF: Charles University, Faculty of Mathematics and Physics, V Holesovickach 2, Prague, 180 00, Czech Republic
AB: Fast forward interplanetary (IP) shocks have been identified as a source of large geomagnetic disturbances. However, the shocks can evolve in the solar wind, they are modified by interaction with the bow shock and during their propagation through the magnetosheath. A few previous papers refer the inclination and deceleration of the IP shock front in this region. Our contribution continues this effort and presents the study of an IP shock interaction with the bow shock. Since the bow shock is a reversed fast shock, the interaction of the IP shock and bow shock is a problem of interaction of two fast MHD shocks. We compare profiles of magnetic field and plasma parameters observed by several spacecraft in the solar wind and magnetosheath with the profiles of the same parameters resulting from the MHD numerical model. The MHD model suggests that the interaction of an IP shock with the bow shock results in an inward bow shock displacement that is followed by its outward motion. Such motion will result in an indentation propagating along the bow shock surface. This scenario is confirmed by multipoint observations. Moreover, the model confirms also previous suggestions on the IP shock deceleration in the magnetosheath.
DE: 2139 Interplanetary shocks
DE: 2154 Planetary bow shocks
DE: 2728 Magnetosheath
DE: 2753 Numerical modeling
DE: 2784 Solar wind/magnetosphere interactions
SC: SPA-Magnetospheric Physics [SM]
MN: 2007 Joint Assembly