TY  - JOUR
A1  - Xue, Zhike
A1  - Yan, Xiaoli
A1  - Cheng, Xin
A1  - Yang, Liheng
A1  - Su, Yingna
A1  - Kliem, Bernhard
A1  - Zhang, Jun
A1  - Liu, Zhong
A1  - Bi, Yi
A1  - Xiang, Yongyuan
A1  - Yang, Kai
A1  - Zhao, Li
T1  - Observing the release of twist by magnetic reconnection in a solar filament eruption
JF  - Nature Communications
N2  - Magnetic reconnection is a fundamental process of topology change and energy release, taking place in plasmas on the Sun, in space, in astrophysical objects and in the laboratory. However, observational evidence has been relatively rare and typically only partial. Here we present evidence of fast reconnection in a solar filament eruption using high-resolution H-alpha images from the New Vacuum Solar Telescope, supplemented by extreme ultraviolet observations. The reconnection is seen to occur between a set of ambient chromospheric fibrils and the filament itself. This allows for the relaxation of magnetic tension in the filament by an untwisting motion, demonstrating a flux rope structure. The topology change and untwisting are also found through nonlinear force-free field modelling of the active region in combination with magnetohydrodynamic simulation. These results demonstrate a new role for reconnection in solar eruptions: the release of magnetic twist.
Y1  - 2016
U6  - https://doi.org/10.1038/ncomms11837
SN  - 2041-1723
VL  - 7
PB  - Nature Publ. Group
CY  - London
ER  - 
TY  - GEN
A1  - Su, Yingna
A1  - Kliem, Bernhard
A1  - van Ballegooijen, Adriaan
A1  - Deluca, Edward
T1  - Numerical simulations of the CME on 2010 April 8
T2  - Solar and Astrophysical Dynamos and Magnetic Activity
N2  - We present 3D zero-beta ideal MHD simulations of the solar flare/CME event that occurred in Active Region 11060 on 2010 April 8. The initial magnetic configurations of the two simulations are stable nonlinear force-free field and unstable magnetic field models constructed by Su et al. (2011) using the flux rope insertion method. The MHD simulations confirm that the stable model relaxes to a stable equilibrium, while the unstable model erupts as a CME. Comparisons between observations and MHD simulations of the CME are also presented.
T3  - Zweitveröffentlichungen der Universität Potsdam : Mathematisch-Naturwissenschaftliche Reihe - 674 
KW  - Sun: coronal mass ejections (CMEs)
KW  - Sun: flares
KW  - Sun: magnetic fields
Y1  - 2019
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-414887
SN  - 1866-8372
IS  - 674
SP  - 575
EP  - 576
ER  -