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- W1505419005 abstract "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." @default.
- W1505419005 created "2016-06-24" @default.
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- W1505419005 date "1996-01-01" @default.
- W1505419005 modified "2023-09-25" @default.
- W1505419005 title "Transition of slow shocks to fast shocks" @default.
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- W1505419005 doi "https://doi.org/10.1063/1.51343" @default.
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