Estimating the Coronal Supra-Arcade Downflow Radio Emission: From Centimeter Through Submillimeter Wavelengths

Supra-arcade downflows (SADs) are infrequent, wiggly, and low-emission structures observed to descend through the solar corona, mostly in EUV soft X-ray frequencies. Based on their physical characteristics, SADs have been interpreted as low-density bubbles related magnetic reconnection processes during long-term erupting flares. In this work, we use numerical MHD simulations compute flux density maps, which convolved with telescope beams synthesize images aim assess expected SAD emission radio wavelengths. We assume that is thermal bremsstrahlung from a fully ionized plasma without any appreciable gyroresonance contribution since fields of order 10 G. find should be optically thin frequency range [10–1,000] GHz, spatially integrated larger than 1 Jy. conclude, therefore, consistently less bright surrounding fan observing frequencies between [0.5–1,000] GHz feasible present instrumentation. The strategies proposed, including instruments can used. Moreover, is, for most part, thin, proportional temperature, density, line-of-sight depth when combined may allow better temperature determination SADs.