Journal
NATURE COMMUNICATIONS
Volume 7, Issue -, Pages -Publisher
NATURE PUBLISHING GROUP
DOI: 10.1038/ncomms11522
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Funding
- 973 program [2012CB825601]
- Chinese Academy of Sciences [KZZD-EW-01-4]
- National Natural Science Foundation of China [41204126, 41231068, 41274192, 41531073, 41374176, 41574170, 41574171]
- Specialized Research Fund for State Key Laboratories
- Youth Innovation Promotion Association of CAS [2015122]
- International Space Science Institute through an International Team
- [NSF-AGS1153323]
- [AGS1062050]
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Solar eruptions are well-recognized as major drivers of space weather but what causes them remains an open question. Here we show how an eruption is initiated in a non-potential magnetic flux-emerging region using magnetohydrodynamic modelling driven directly by solar magnetograms. Our model simulates the coronal magnetic field following a long-duration quasi-static evolution to its fast eruption. The field morphology resembles a set of extreme ultraviolet images for the whole process. Study of the magnetic field suggests that in this event, the key transition from the pre-eruptive to eruptive state is due to the establishment of a positive feedback between the upward expansion of internal stressed magnetic arcades of new emergence and an external magnetic reconnection which triggers the eruption. Such a nearly realistic simulation of a solar eruption from origin to onset can provide important insight into its cause, and also has the potential for improving space weather modelling.
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