Modelling X-ray and radio emission from a flaring T-Tauri star

T-Tauri stars exhibit strong flaring activity. These flares are over-luminous in radio compared with X-rays, deviating from the well-known Gudel-Benz relation. This has been previously been interpreted by considering the flares to take place in large loops interacting with the inner radius of the accretion disk, with gyrosynchrotron emission mainly from a population of non-thermal electrons created by magnetic reconnection (Waterfall et al, Mon. Not. Roy Ast. Soc., 483, 917, 2019).  We present  new results of time-dependent modelling of the radio emission from a flaring T-Tauri star, using three-dimensional magnetohydrodynamic simulations combined with a model for non-thermal electrons in magnetic loops and radiative transfer modelling of the gyrosynchrotron emission (Waterfall et al, Mon. Not. Roy Ast. Soc., 496, 2715, 2020. We predict the multi-frequency  (1  - 1000 GHz) time variation intensity and circular polarisation of the radio emission. We show that observations of the time varying spectrum and polarisation could place important constraints on the  physical properties of the flare environment and the accretion process.