Physics
Scientific paper
Jul 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aipc..382..562w&link_type=abstract
Proceedings of the eigth international solar wind conference: Solar wind eight. AIP Conference Proceedings, Volume 382, pp. 562
Physics
Planetary Bow Shocks, Interplanetary Shocks, Magnetohydrodynamics And Plasmas
Scientific paper
As a CME pushes its way through preceding slower solar wind, large disturbances in the interaction region may evolve to form transient MHD shocks. The shocks can be slow shocks in the coronal space but they appear as fast shocks near 1 AU. We use a MHD model to study the transition of slow shocks to fast shocks in an interaction region sandwiched between a faster solar wind and a slower solar wind near the equatorial plane. The transition process is attributed chiefly to the radial increase of β, and to a lesser degree to the radial increase of the shock angle θ. Under the initial condition of small β and θ near 0.1 AU, the interaction region evolves to form a pair of slow shocks inside 0.15 AU. As the interaction region convects outward, the increases of β and θ cause a transition of the shock system between 0.15 and 0.3 AU from a slow shock pair to a double shock pair. As the system moves outward, β and θ continue to increase, the fast shock grows stronger, and the slow shock becomes weaker. Eventually, the slow shocks fade away, and the shock system evolves to a pair of fast shocks.
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