Computer Science
Scientific paper
Jul 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aipc..382..457o&link_type=abstract
Proceedings of the eigth international solar wind conference: Solar wind eight. AIP Conference Proceedings, Volume 382, pp. 457
Computer Science
1
Solar Wind Plasma, Sources Of Solar Wind, Planetary Bow Shocks, Interplanetary Shocks, Magnetohydrodynamics And Plasmas
Scientific paper
The interaction of an interplanetary shock with the heliospheric plasma sheet (HPS) is simulated using the 2 12D MHD model in the meridional plane. The shock structure is generated by a velocity pulse and consists of a strong broad forward shock (FS) with a concave shape and a much weaker and narrower reverse shock (RS) with a convex shape. The flat equatorial HPS, with its larger mass density and slower flow velocity, modifies this shock structure. A dimple is formed at the FS and a reverse dimple is formed at the RS. A large distortion of the heliospheric current sheet (HCS) occurs when the velocity pulse is introduced outside the HPS. The interaction of a shock with the HPS leads to very large southward values of the interplanetary magnetic field due to an effect of shock compression, field-line draping, and deflection of the HCS.
Dryer Murray
Odstrcil Dusan
Smith Zdenka
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