Synthetic Radio Imaging for Quiescent and CME-flare Scenarios

TL;DR

This paper introduces a new synthetic radio imaging tool that simulates Bremsstrahlung emission in the solar corona, integrating with MHD simulations to improve understanding of solar radio phenomena.

Contribution

The paper presents a novel synthetic radio imaging method that works with MHD simulations and includes ray-tracing with refraction effects for solar radio emission modeling.

Findings

Results agree with observed solar radio emissions.

Refraction significantly affects source localization.

Ray-tracing improves accuracy of emission source imaging.

Abstract

Radio observations grant access to a wide range of physical processes through different emission mechanisms. These processes range from thermal and quiescent to eruptive phenomena, such as shock waves and particle beams. We present a new synthetic radio imaging tool that calculates and visualizes the Bremsstrahlung radio emission. This tool works concurrently with state-of-the-art Magnetohydrodynamic (MHD) simulations of the solar corona using the code BATS-R-US. Our model produces results that are in good agreement with both high and low frequency observations of the solar disk. In this study, a ray-tracing algorithm is used and the radio intensity is computed along the actual curved ray trajectories. We illustrate the importance of refraction in locating the radio emitting source by comparison of the radio imaging illustrations when the line-of-sight instead of the refracted paths are considered. We are planning to incorporate non-thermal radio emission mechanisms in a future version of the radio imaging tool.