Interplanetary shock shapes: comparison of local and global parameters

Details Interplanetary shock shapes: comparison of local and global parameters Interplanetary shock shapes: comparison of local and global parameters

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh23b1644k&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SH23B-1644

Other

2101 Coronal Mass Ejections (7513), 2102 Corotating Streams, 2139 Interplanetary Shocks

Scientific paper

We are presenting a study of the shapes of interplanetary shocks observed by multiple spacecraft. The shock normal orientation and propagation speed are calculated locally from the magnetic field and plasma measurements of the Wind spacecraft by applying the Koval and Szabo [2008] technique which uses the isotropic Rankine-Hugoniot (RH) conservation equations. We have modified the technique by applying the anisotropic and multi-ion RH conservation equations in order to improve the accuracy of the calculated parameters. These local parameters are consequently used to predict the times of the shock arrival to the locations of the other spacecraft available in the solar wind assuming shock planarity and constant propagation speed. We compare the predicted times with those observed as well as compare the Wind local shock normal orientation and propagation speed with the corresponding global parameters determined from the four-spacecraft locations and times of the shock passages (when available). The agreement of the shock shapes with the planar assumption is discussed based on the shock drivers. We also discuss the influence of temperature anisotropy and alpha-particle parameters on the accuracy of the locally calculated shock parameters. Determining the true orientation of CME-driven shocks is important for a better understanding of particle acceleration processes.

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