Speaker
Description
Decaying magnetohydrodynamic (MHD) turbulence is important in various astrophysical contexts,
including early universe magnetic fields, star formation, turbulence in galaxy clusters,
magnetospheres and solar corona. I will talk about how decaying MHD turbulence displays the
phenomenon of inverse energy transfer. Our work has uncovered the important role of magnetic
reconnection in driving such inverse transfer. Further, we found that both 2D and 3D simulations
show similar power law exponents. To understand this intriguing similarity, we investigated the
possible quasi-two-dimensionalization of the 3D system. I will talk about our efforts to understand
the nature of this quasi-two-dimensionalization. Finally, I will present a quasi-2D hierarchical
merger model which recovers the relevant power law scalings.
