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• W2032102567 startingPage "99" @default.
• W2032102567 abstract "We present results from 3D visco-resistive magnetohydrodynamic (MHD) simulations of the emergence of a convection zone magnetic flux tube into a solar atmosphere containing a pre-existing dipole coronal field, which is orientated to minimize reconnection with the emerging field. We observe that the emergence process is capable of producing a coronal flux rope by the transfer of twist from the convection zone as found in previous simulations. We find that this flux rope is stable, with no evidence of a fast rise, and that its ultimate height in the corona is determined by the strength of the pre-existing dipole field. We also find that although the electric currents in the initial convection zone flux tube are almost perfectly neutralized, the resultant coronal flux rope carries a significant net current. These results suggest that flux tube emergence is capable of creating non-current-neutralized stable flux ropes in the corona, tethered by overlying potential fields, a magnetic configuration that is believed to be the source of coronal mass ejections." @default.
• W2032102567 created "2016-06-24" @default.
• W2032102567 creator A5043026249 @default.
• W2032102567 creator A5067791862 @default.
• W2032102567 creator A5070140449 @default.
• W2032102567 date "2013-11-08" @default.
• W2032102567 modified "2023-10-13" @default.
• W2032102567 title "SIMULATIONS OF EMERGING MAGNETIC FLUX. I. THE FORMATION OF STABLE CORONAL FLUX ROPES" @default.
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• W2032102567 doi "https://doi.org/10.1088/0004-637x/778/2/99" @default.
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