Speaker
Description
In this presentation, we will explore the fundamental properties of magnetic reconnection, with a particular emphasis on the complexities of three-dimensional (3D) reconnection and the differences with two-dimensional (2D) scenarios. We will present recent state-of-the-art numerical simulations that show how 3D reconnection is key to understanding a variety of phenomena such as braiding, nanojets, and the heating of fundamental blocks in the atmosphere such as Coronal Bright Points, moreover including observations to support the theoretical findings. Additionally, we will address the implications of the differing Prandtl number in simulations versus the actual solar atmosphere. We will also discuss the challenges that need to be addressed in the near future both from theory and observations, and the potential opportunities from future missions such as MUSE and Solar-C.
