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Solar energetic particles (SEPs) are accelerated by magnetic reconnection-driven processes during solar flares and by CME-driven shocks. Large gradual SEP events, associated with high-energy protons (up to tens of GeV), can cause hazardous space weather conditions at Earth and hence pose a severe radiation risk for crewed spaceflight and a significant threat to near-Earth technological assets. To mitigate the risk posed by SEPs and solar eruptive events we must be able to forecast these events prior to their occurrence. Achieving this task is very difficult because it requires a multidisciplinary approach combining a broad range of remote and in-situ observations, data-driven modelling and simulations. One of the main issues is what input parameters, in particular magnetic field properties of source regions taken from solar observations, are required to improve forecasts provided by data-driven models. This is one of the aims of NERC’s “SWIMMR Aviation Risk Monitoring” (SWARM) project.
In this meeting we aim to discuss the configuration and evolution of the solar magnetic field in the build-up to solar eruptive events as well as the production and propagation of solar energetic particles. What magnetic field parameters would be useful for the next generation of space weather models to predict solar energetic particles and their associated flares and coronal mass ejections? What effect do the solar and heliospheric magnetic fields have on the acceleration, injection and propagation of energetic particles? The timing of this meeting is particularly appropriate given the ongoing SWARM project and the availability of data from new missions such as Parker Solar Probe and Solar Orbiter.
Stephanie Yardley (UCL/MSSL)
Lucie Green (UCL/MSSL)
Charlotte Waterfall (UCLan)
Silvia Dalla (UCLan)
Book a Fellows May SDM Online ticket
Book a Non Fellows May SDM Online Ticket