Physics
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh62a06s&link_type=abstract
American Geophysical Union, Spring Meeting 2001, abstract #SH62A-06
Physics
2111 Ejecta, Driver Gases, And Magnetic Clouds, 2134 Interplanetary Magnetic Fields, 2139 Interplanetary Shocks, 2164 Solar Wind Plasma
Scientific paper
Fast moving magnetic clouds tend to drive interplanetary shocks that take energy out of the propagating structure. As the magnetic clouds travel through the interplanetary medium they encounter a variable solar wind background. Using multi-spacecraft observations primarily from ACE and WIND, and from IMP 8 and Geotail when available, the 3-dimensional shape of interplanetary shocks driven by magnetic clouds on the hundred Earth radii scale will be discussed. The complete magnetic field and solar wind ion data sets were used to calculate the local shock surface normals and speeds, along with their associated uncertainties, by fitting the shocks with a full non-linear least squares "Rankine-Hugoniot" technique. Multi-spacecraft results reveal that on the distance scale of ACE's L1 halo orbit the shocks deviate from a simple planar geometry even when driven by such large structures as magnetic clouds. This result has important consequences for the determination of magnetic cloud propagation and expansion rate. It appears that to first order magnetic clouds have sufficient internal magnetic energy to maintain their flux rope profile and that the driven shocks will change their shapes to adjust to the local ambient solar wind conditions.
Paularena Karolen I.
Skoug Ruth M.
Smith Walter C.
Szabo Andras
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