Origins of Electron Heating from their Velocity Distributions in Weakly Collisional Plasmas

M. Hasan Barbhuiya, Ph.D.

Often called the fourth state of matter, plasmas make up nearly all visible matter in the universe, from the Sun’s surface to the distant intergalactic medium. Yet, the processes that heat these vast, nearly collisionless plasmas remain one of the most intriguing puzzles in space and astrophysical physics. In this talk, we will explore how the motion of individual electrons with different velocities, called “velocity distributions”, holds the key to understanding their heating. Using “magnetic reconnection”, a process where magnetic field lines break and reconnect, as a natural example of energy conversion in plasmas which transforms magnetic energy into plasma heat, we will cover how electrons can get heated even when collisions are rare. We will first examine a key mechanism used to study heating and then discuss the newer approach of analyzing heating through the lens of velocity distributions. By connecting these two perspectives, we will reveal how uniquely structured electron velocity distributions drive the production of hot, energetic electrons that could influence space weather and may shape astrophysical phenomena.

To participate in this event virtually via Zoom, go to https://uiowa.zoom.us/j/95662833839?from=addon.