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Paper: Breakout Coronal Mass Ejection or Streamer Blowout: the Bugle Effect
Volume: 429, Numerical Modeling of Space Plasma Flows, Astronum-2009
Page: 219
Authors: van der Holst, B.
Abstract: This proceedings paper is mostly based on a much longer research paper van der Holst et al. (2009). We present three-dimensional magnetohydrodynamic simulations of coronal mass ejections (CMEs) initiated by the breakout mechanism. The initial steady state solar wind contains a central breakout arcade with magnetic field lines that are oppositely oriented to the overarching helmet streamer. This configuration has a magnetic null on the leading edge of the central breakout arcade. By applying shear flow near the central polarity inversion line at the coronal base, the field near the null starts to reconnect and removes the overlying helmet streamer field. During the erupting, the plasma ahead of the arcade is swept up. The helmet streamer swells up and the width of the streamer follows a “bugle” pattern in time. If the streamer swelling is sufficient, the breakout reconnection will succeed all the way to the top of the helmet streamer, resulting in a fast breakout CME.
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