Statistics – Computation
Scientific paper
Mar 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.477..263p&link_type=abstract
In: Proceedings of the Second Solar Cycle and Space Weather Euroconference, 24 - 29 September 2001, Vico Equense, Italy. Editor:
Statistics
Computation
3
Cmes, Magnetic Clouds, Mhd Shocks, Numerical Simulations
Scientific paper
The shocks in the solar corona caused by fast Coronal Mass Ejections (CMEs) and the shock at the Earth's magnetosphere caused by the corresponding magnetic clouds (superposed on the solar wind) are studied in the framework of computational magnetohydrodynamics (MHD). Due to the presence of three characteristic velocities and the anisotropy induced by the magnetic field, MHD shocks can have a complicated structure including secondary shock fronts, overcompressive and compound shocks, etc. Numerical simulations show that CME shocks (in the lower corona) and the shock at the Earth's magnetosphere (at times of the impact of a magnetic cloud) have such a complex structure. The CME shocks are important for 'space weather' because they can easily be observed in radio wavelengths. This makes it possible to track the position of the CMEs/magnetic clouds and, hence, to follow their propagation through the corona. The collision of two such shocks is discussed. Also, the possibility of locating the magnetic cloud from the passage of a satellite through the leading shock front is discussed. Moreover, the topology of the shock at the Earth's magnetosphere at the impact of a magnetic cloud is important for the 'geo-effectiveness' of the magnetic storms. Hence, a detailed study of the MHD shocks generated by CMEs may reveal some of the key properties space weather.
Csik Arpad
de Sterck Hans
Deconinck H.
der Holst Bart van
Milesi A.
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