Speaker
Description
The origin of radio emission in radio-quiet AGN remains a central debate regarding the nature of accretion and feedback around supermassive black holes. While this emission is often attributed to star formation or diffuse outflows, current evidence increasingly points toward a compact jet base or a magnetized corona tied to the sub-parsec accretion engine. The most definitive diagnostic for identifying these processes lies in comparing radio and X-ray flux variations, as correlated or lagged variability provides compelling evidence of a direct physical connection between the two components. In this talk, I present a systematic investigation of the radio variability properties of radio-quiet AGN, a territory that remains largely unexplored. These sources exhibit a diverse range of amplitudes and timescales, and I examine how these properties scale with Eddington ratios and black hole masses. By comparing these results with X-ray light curves, I discuss how specific time lags may indicate a synchrotron jet nature similar to the behavior observed in X-ray binaries.