期刊
ASTROPHYSICAL JOURNAL
卷 778, 期 2, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/778/2/99
关键词
magnetohydrodynamics (MHD); Sun: coronal mass ejections (CMEs); Sun: magnetic fields
资金
- NASA Living With a Star and Solar and Heliospheric Physics programs
- ONR 6.1 Program
- NRL-Hinode analysis program
- UK Space Agency [ST/J001732/1] Funding Source: researchfish
- Div Atmospheric & Geospace Sciences
- Directorate For Geosciences [1135432] Funding Source: National Science Foundation
We present results from three-dimensional visco-resistive magnetohydrodynamic 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.
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