Modelling an X-class solar are combining observations, electron beam transport physics and MHD numerical simulations

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Background Information: Solar flares are sudden and large explosions of energy caused by the reconnection of magnetic field lines on the Sun's surface. The energy released spans the full range of the electromagnetic spectrum. X-class flares are the most powerful class of solar flare, and this research proposal will explore one of the most unique observations ever taken of an X-class flare, lasting for 1 hour on 10-June-2014, offering bespoke images and spectral diagnostics at incredible spatial and temporal resolution. The flare ribbons imaged are intensely bright, signifyingthe collision of powerful electron beams that traverse from the relatively low plasma density solar corona into the relatively high-density chromosphere below, leading to Bremsstrahlung radiation. The chromosphere responds to this beam injection by rapidly heating and expanding into post-flare magnetic arcades filling the loops with high-speed counter-flowing dense plasma, giving rise to a wide range of plasma fluid instabilities. We can constrain the physical processes in solar flares by diagnosing and forward modeling the highly-resolved spectral observations, assimilating them into numerical models of plasma flows, and deriving electron beam properties.Aims and Objectives: In this project, we will use a unique observation at the highest resolution of a rarely observed X-class mentioned previously to improve our comprehension of plasma physics processes in solar flares. The project will work in two stages. The first stage will involve a detailed exploration of the rapidly evolving large-scale flare phenomenon using coordinated space and ground-based multi-instrument observations spanning a wide range of absorption and emission spectral lines in the near-IR, visible, (E)UV, and X-ray wavelength channels. The insightsgained from this data analysis will allow us to develop sophisticated models of the electron beam transport leading to the flare ribbon formation, as well as to initialize advanced 3D MHD simulations of the chromospheric response to the flare ribbon formation.1 Exploration of are ribbon formation and evolution: The researcher will learn image processing techniques and explore the Swedish 1-m Solar Telescope (SST) and Solar Dynamics Observatory (SDO) image and spectral observations of the are ribbon formation, utilizing 3D visualization software. These will be used to characterize the flare ribbons' statistical properties and dynamic behaviour.2 Electron beam transport modelling incorporating observations of X-ray signatures during the flare-X-ray signatures from RHESSI observations of the flare that capture emissions near the source of the electron beam acceleration site will be forward-modelled using object-based spectroscopy software. This will allow us to examine the electron flux properties near the loop tops in the corona and during ribbon formation in the chromosphere. The results derived from objective one shall be used to model the transport and energy deposition of electrons. 3 3D MHD modelling of post-flare loop formation: Using the observationally derived properties from Objective one and two, the researcher will develop advanced 3D MHD models of plasma flows and instabilities in curved loop simulations using the numerical code Lare3D. We shall be modeling the plasma processes in a solar loop in the form of a half-torus and presenting the data in the format of an observing platform(forward modelling).