Structure and Dynamics of Magnetic Fields in the Sun, Solar System and Beyond
Sequential eruptions triggered during the early phase of flux emergence under a circular filament - observations and modelling
Sally Dacie
Tibor Török (Predictive Science Inc.), Mark Linton (Naval Research Laboratory), Pascal Démoulin (Observatoire de Paris), Lidia van Driel-Gesztelyi (UCL MSSL, Observatoire de Paris, Konkoly Observatory), David Long (UCL MSSL))
UCL Mullard Space Science Laboratory
The emergence of magnetic flux through the solar photosphere in the vicinity of a filament can trigger a coronal mass ejection (CMEs), or alternatively it could stabilise the filamentary structure. Both modelling and observational studies have shown that whether a filament is activated depends on the position, orientation and strength of the emerging flux. The emergence of a small bipole underneath a quiescent circular filament on 18-July-2014 causes the filament to split, to erupt and in the process to form a new filament arcade, which also undergoes an eruption. We propose a mechanism to explain this activity, based on SDO/AIA and HMI observations, and we are currently working on simulations to reproduce this.


16:30 - 18:00
EX - C33 (150)