Le 1 avril 2016
De 10h30 à 12h00
Tomasz Rembiasz
Université de Valence
Magnetorotational instability (MRI) is one of the most promising agents significantly amplifying magnetic fields in (resulting from rapidly rotating progenitors) core-collapse supernovae (CC-SNe). The initial phase of the MRI (of the exponential growth) is well understood, however its exact termination mechanism remains unknown. In this talk, we present our newest results clearly indicating that the MRI, given CC-SN conditions, is terminated by the parasitic Kelvin-Helmholtz instability. This allows us to set the limit on the maximum magnetic field amplification by the MRI.