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The eruption of a small-scale emerging flux rope as the driver of an M-class flare and a coronal mass ejection View all abstracts by submitter

Xiaoli Yan   Submitted: 2017-07-08 10:19

Solar flares and coronal mass ejections (CMEs) are the most powerful explosions in the Sun. They are major sources of potentially destructive space weather conditions. However, the possible causes of their initiation remain controversial. By using high resolution data observed by NST of BBSO, supplemented by Solar Dynamics Observatory (SDO) observations, we present unusual observations of a small-scale emerging flux rope near a large sunspot, whose eruption produced an M-class flare and a coronal mass ejection. The presence of the small-scale flux rope was indicated by static nonlinear force free field (NLFFF) extrapolation as well as data-driven MHD modeling of the dynamic evolution of the coronal 3D magnetic field. During the emergence of the flux rope, rotation of satellite sunspots at the footpoints of the flux rope was observed. Meanwhile, the Lorentz force, magnetic energy, vertical current, and transverse fields were increasing during this phase. The free energy from the magnetic flux emergence and twisting magnetic fields is sufficient to power the M-class flare. These observations for the first time present the complete process from the emergence of the small-scale flux rope to the production of solar eruptions.

Authors: X.L. Yan, C.W. Jiang, Z.K. Xue, J.C. Wang, E.R. Priest, L.H. Yang, D.F. Kong, W.D. Cao, H.S. Ji
Projects: BBSO/NST

Publication Status: accepted for publication in ApJ.
Last Modified: 2017-07-11 11:23
Go to main E-Print page  Elongation of Flare Ribbons  Magnetic Flux Cancelation as the Origin of Solar Quiet Region Pre-Jet Minifilaments  Edit Entry  Download Preprint  Delete Entry 

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