TY  - GEN
A1  - Driel-Gesztelyi, L. van
A1  - Baker, Daniel N.
A1  - Török, Tibor
A1  - Pariat, Etienne
A1  - Green, L. M.
A1  - Williams, D. R.
A1  - Carlyle, J.
A1  - Valori, G.
A1  - Démoulin, Pascal
A1  - Matthews, S. A.
A1  - Kliem, Bernhard
A1  - Malherbe, J.-M.
T1  - Magnetic reconnection driven by filament eruption in the 7 June 2011 event
T2  - Postprints der Universität Potsdam : Mathematisch Naturwissenschaftliche Reihe
N2  - During an unusually massive filament eruption on 7 June 2011, SDO/AIA imaged for the first time significant EUV emission around a magnetic reconnection region in the solar corona. The reconnection occurred between magnetic fields of the laterally expanding CME and a neighbouring active region. A pre-existing quasi-separatrix layer was activated in the process. This scenario is supported by data-constrained numerical simulations of the eruption. Observations show that dense cool filament plasma was re-directed and heated in situ, producing coronal-temperature emission around the reconnection region. These results provide the first direct observational evidence, supported by MHD simulations and magnetic modelling, that a large-scale re-configuration of the coronal magnetic field takes place during solar eruptions via the process of magnetic reconnection.
T3  - Zweitveröffentlichungen der Universität Potsdam : Mathematisch-Naturwissenschaftliche Reihe - 608 
KW  - MHD
KW  - instabilities
KW  - Sun: activity
KW  - magnetic fields
KW  - coronal mass ejections (CMEs)
KW  - filaments
KW  - methods: numerical
KW  - data analysis
Y1  - 2019
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-415671
IS  - 608
SP  - 502
EP  - 503
ER  - 
TY  - GEN
A1  - Kliem, Bernhard
A1  - Rust, S.
A1  - Seehafer, Norbert
T1  - Helicity transport in a simulated coronal mass ejection
T2  - Postprints der Universität Potsdam : Mathematisch Naturwissenschaftliche Reihe
N2  - It has been suggested that coronal mass ejections (CMEs) remove the magnetic he-licity of their coronal source region from the Sun. Such removal is often regarded to be necessary due to the hemispheric sign preference of the helicity, which inhibits a simple annihilation by reconnection between volumes of opposite chirality. Here we monitor the relative magnetic he-licity contained in the coronal volume of a simulated flux rope CME, as well as the upward flux of relative helicity through horizontal planes in the simulation box. The unstable and erupting flux rope carries away only a minor part of the initial relative helicity; the major part remains in the volume. This is a consequence of the requirement that the current through an expanding loop must decrease if the magnetic energy of the configuration is to decrease as the loop rises, to provide the kinetic energy of the CME.
T3  - Zweitveröffentlichungen der Universität Potsdam : Mathematisch-Naturwissenschaftliche Reihe - 569 
KW  - magnetic fields
KW  - MHD
KW  - coronal mass ejections
KW  - magnetohydrodynamics
KW  - sun
Y1  - 2019
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-412907
SN  - 1866-8372
IS  - 569
SP  - 125
EP  - 128
ER  -