Applied Mathematics Seminars: What can test particles tell us about magnetic reconnection in the solar corona?
15 December 2017 14:00 in CM219
Solar flares are highly explosive events which release significant quantities of energy (up to 10^32 ergs) from specific magnetic configurations in the solar atmosphere. As part of this process, flares produce unique signatures across the entire electromagnetic spectrum, from radio to ultra-violet (UV) and X-ray wavelengths, over extremely short length and timescales. Many of the observed signals are indicative of strong particle acceleration, where highly energised electron and proton populations rapidly achieve MeV/GeV energies and therefore form a significant fraction of the energy budget of each event. It is almost universally accepted that magnetic reconnection plays a fundamental role (on some level) in the acceleration of particles to such incredible energies.
In this talk, I will briefly summarise a series of recent experiments where test particles are introduced into a number of 3D magnetic reconnection configurations. I will discuss the particle population response to each configuration and what these responses might infer for both simulations and observations of magnetic reconnection in the flaring solar corona.
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