Speaker
Description
We present an end-to-end, physics-based forward model for type-IV solar radio bursts that links coronal dynamics, particle transport, and radio emission in one pipeline. We first use the 3D coronal MHD model COCONUT to produce a realistic background and drive a CME as an unstable, modified Titov–Démoulin magnetic-flux-rope. We then inject energetic electrons and evolve their distributions with the test-particle transport code PARADISE. Finally, we pass the time-dependent electron and plasma parameters to the Ultimate Fast Gyrosynchrotron Codes (UFGSCs) to compute line-of-sight emissivities and synthetic spectra.
This workflow reproduces hallmark type-IV behavior: electrons injected near the flux-rope core remain largely confined, yielding long-lived gyrosynchrotron continua; intensities and durations depend strongly on viewing geometry and on CME/electron properties; and the brightest emission typically originates from the CME flanks. As the flux rope expands and its magnetic field weakens, the spectral peak drifts to lower frequencies, consistent with observations.
By coupling COCONUT → PARADISE → UFGSCs, we provide a practical way to interpret type-IV spectra and to constrain the magnetic content and geometry of CMEs directly from radio data.
