Speaker
Description
First Name: Vaggelis
Last Name: Karantanis
Affiliation: University of Ioannina
All Authors: Vaggelis Karantanis, Vasilis Archontis, Juxhin Zhuleku, Kostas Moraitis
Abstract: In the solar atmosphere there are a wide range of dynamic eruptive phenomena like jets, flares and coronal mass ejections (CMEs). It is believed that those phenomena result from the interaction of magnetic fields emerging from the convection zone and interact with the pre-existing magnetic field in the corona. We model flux emergence by performing 3D magnetohydrodynamic (MHD) simulations of twisted flux tubes using the Lare3D code. We examined two different geometries, a horizontal and a toroidal magnetic flux tube. For both horizontal and toroidal flux tubes we used the same initial conditions for the solar stratification as well as the same characteristics of the tube itself. An important prerequisite for the eruptions is an adequate amount of magnetic flux along the axis of the tube. The toroidal flux tube displays twice as many eruptions as the horizontal while also being able to compensate for the axial flux that it looses with each eruption. Nevertheless the horizontal flux tube still manages to transport a larger amount of axial flux, which can make it more effective in describing explosive phenomena observed in the Sun.