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- W2034370974 abstract "[1] We present a three-dimensional (3-D) numerical ideal magnetohydrodynamics (MHD) model, describing the time-dependent expulsion of plasma and magnetic flux from the solar corona that resembles a coronal mass ejection (CME). We begin by developing a global steady-state model of the corona and solar wind that gives a reasonable description of the solar wind conditions near solar minimum. The model magnetic field possesses high-latitude coronal holes and closed field lines at low latitudes in the form of a helmet streamer belt with a current sheet at the solar equator. We further reproduce the fast and slow speed solar wind at high and low latitudes, respectively. Within this steady-state heliospheric model, conditions for a CME are created by superimposing the magnetic field and plasma density of the 3-D Gibson-Low flux rope inside the coronal streamer belt. The CME is launched by initial force imbalance within the flux rope resulting in its rapid acceleration to a speed of over 1000 km/s and then decelerates, asymptotically approaching a final speed near 600 km/s. The CME is characterized by the bulk expulsion of ∼1016 g of plasma from the corona with a maximum of ∼5 × 1031 ergs of kinetic energy. This energy is derived from the free magnetic energy associated with the cross-field currents, which is released as the flux rope expands. The dynamics of the CME are followed as it interacts with the bimodal solar wind. We also present synthetic white-light coronagraph images of the model CME, which show a two-part structure that can be compared with coronagraph observations of CMEs." @default.
- W2034370974 created "2016-06-24" @default.
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- W2034370974 date "2004-01-01" @default.
- W2034370974 modified "2023-10-18" @default.
- W2034370974 title "Three-dimensional MHD simulation of a flux rope driven CME" @default.
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- W2034370974 doi "https://doi.org/10.1029/2002ja009672" @default.
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