Speaker
Description
First Name: Angelos
Last Name: Giannis
Affiliation: University of Ioannina, Greece
All Authors: Angelos Giannis and Vasilis Archontis
Abstract: The formation of magnetohydrodynamic (MHD) shock waves and the viscous heating deposited at them are studied in a three-dimensional (3D) bipolar active region in the Sun. We perform a compressible, resistive MHD simulation of magnetic flux emerging into the magnetized corona from the convection zone. Initially, numerous slow-mode shocks form and propagate upwards in the corona in a highly dynamical manner due to plasmoid ejections from the current sheet. These shocks exhibit a complicated 3D structure and their passage results in profound, transient heating in the corona. The main reconnection event that ensues launches a pair of bidirectional outflows that eject plasmoids. Both of these outflows terminate with two fast-mode MHD shocks as the plasmoids collide and reconnect with the open field lines and the Post-Flare Loops (PFLs). The 3D shock isosurfaces are of elongated shape and viscous dissipation is deposited on them in a non-trivial manner. The fast shock atop the PFLs is associated with a significant temperature increase in the field lines of the loops, linking the the plasmoid ejection with the flaring process.