Magnetic Loops on the Sun

Magnetic spots on Sun like stars are a major driver of space weather and can impact habitability of planets. Sunspots are formed in the interior of the Sun starting in the convection zone where the differential rotation creates pressure causing the loops to become buoyant enough to rise to the photosphere. The formation of sunspots progenitors has been modeled using 3D magnetohydrodynamic simulation of stellar convection. These buoyant magnetic loops are small coherent structures in a large turbulent volume, therefore making the loops hard to find. Here we report on a project to develop and empower post-processing tools for there simulated data sets. We have located almost 200 loops between $0.90 R_{\odot}$ to $0.98R_{\odot}$ and have begun to track their motion through the convection zone.