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Paper: Numerical Experiments on the Two-Step Emergence of Solar Magnetic Fields from the Convective Layer
Volume: 454, The 3rd Hinode Science Meeting
Page: 259
Authors: Toriumi, S.; Yokoyama, T.
Abstract: We perform two-dimensional magnetohydrodynamic (MHD) simulations of the flux emergence from the solar convection zone to the corona. The flux sheet is initially located moderately deep (–20,000 km) in the adiabatically stratified convection zone and is perturbed to trigger the Parker instability. The flux rises through the interior, but decelerates around the strongly sub-adiabatic photosphere. As the magnetic pressure gradient increases, the flux becomes unstable to the Parker instability again so that further evolution to the corona occurs. We show the results of the simulations based on this ‘two-step emergence’ model and make some discussions in connection with the results of the thin-flux-tube simulations.
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