Advisors: Dibyendu Nandi & Richard Canfield
Solar active regions, consisting of sunspots, are areas of concentrated magnetic fields on the solar surface that are formed as a result of the buoyant eruption of magnetic flux tubes from the interior of the Sun. The magnetic fields within these active regions are known to be twisted. The magnitude and distribution of active region twists can give us important information about the dynamics of the underlying flux tube constituting the sunspots. Twisted magnetic fields also store energy, which can be released through solar eruptions such as Flares or Coronal Mass Ejections. Observational measurements and analysis of active region twist distribution are therefore important for understanding many aspects of solar dynamics.
In this project, the student will learn how to quantify magnetic field twist through the reduction and analysis of solar magnetogram instrument data using softwares and numerical techniques. Subsequently, statistical data analysis will be used to infer the details of this twist distribution and understand its implications for magnetic flux tube dynamics and solar eruptive activity. The student should have some experience with computers and numerical techniques. Prior experience with IDL is desirable, but not essential. This project is the continuation of Chris Lowder's project from last summer: click here for his research logbook and final presentation.