Numerical Analysis Seminars: Connecting Solar Coronal Holes and Open Magnetic Flux through Observation and Models of Solar Cycles 23 and 24
11 December 2015 14:00 in CM105
At the heart of the sun, massive densities of plasma drive the processes that give rise to the illumination of our solar system. Magnetic fields are generated from the motion of this plasma, rising and extending into the ‘atmosphere’ of the sun, the solar corona. Coronal holes, dark patches appearing in extreme ultraviolet and x-ray data, often coincide with the roots of magnetic field lines that extend outward into the heliosphere. These open magnetic structures provide a source of the fast solar wind and heliospheric open magnetic flux. Coronal holes provide a useful observational proxy for studying these properties in depth.
Through the use of multiple spacecraft datasets spanning the past 18 years (spanning over one and one-half solar activity cycles), we have mapped and characterised these coronal holes. With a numerical model to drive the surface magnetic field over a corresponding span, the open magnetic field structure can be computed. In comparison with observed coronal hole patterns, new constraints are placed on model parameters.
Contact David.Bourne@durham.ac.uk for more information