01/14/2022
By Lynne Schaufenbil
Abstract: The evolution of the magnetic field in the solar corona is mainly driven by the activities at the photospheric level, where active regions are the primary source of magnetic flux. The shearing motion of photospheric plasma due to differential rotation and the twist of the emerging active regions generates global and local non-potentiality in the coronal magnetic field. Magnetofrictional models are capable of reproducing the quasi-static evolution of the coronal magnetic field as well as identifying structures prone to eruption. In this presentation, I will talk about the coronal magnetic field evolution during two phases of the solar cycle: the minimum and the maximum.
Bhowmik is a post-doctoral research associate in the Department of Mathematical Sciences, Durham University, UK. "I am working with Prof. Anthony Yeates on computational modelling of the magnetic field in solar corona based on a magneto-frictional approach to determine the role of memory in building up coronal magnetic structures, and the possible observational consequences. I did my Ph.D. under the supervision of Prof. Dibyendu Nandy. The primary goal of my research work during Ph.D. was to understand and predict the short-term as well as long-term variability of the Sun’s large-scale magnetic field by utilising computational models."
Please contact Lynne Schaufenbil for the Zoom link if you wish to attend.