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The mechanism and the region of generation of variable continuum emission are poorly understood for radio‐loud active galactic nuclei because of the complexity of the nuclear region. High‐resolution radio very long baseline interferometry (VLBI) observations have allowed us to zoom into a subparsec‐scale region of the jet in the radio‐loud galaxy 3C 390.3. We have combined the radio VLBI and the optical data covering the time period of 14 yr in order to look for a link between the optical flares and the parsec‐scale jet. We have identified two stationary and nine moving radio features in the innermost subparsec‐scale region of the jet. All nine ejections are associated with optical flares. We have found a significant correlation (at a confidence level of &gt;99.99 per cent) between the ejected jet components and the optical continuum flares. The epochs at which the moving knots pass through the location of a stationary radio feature and at which the optical light curve reaches maximum are correlated. The radio events follow the maxima of optical flares with a mean time delay of  0.10 ± 0.04 yr . This correlation can be understood if the variable optical continuum emission is generated in the innermost part of the jet. A possible mechanism of the energy release is the ejection of knots of high‐energy electrons that are accelerated in the jet flow and generate flares of synchrotron continuum emission in the wide range of frequencies from radio to X‐ray bands. In this scenario, the beamed optical continuum emission from the jet and counterjet ionizes a gas in a subrelativistic outflow surrounding the jet. This results in the formation of two outflowing conical regions with broad emission lines (in addition to the conventional broad‐line region around the central nucleus).

Observational evidence for the link between the variable optical continuum and the subparsec‐scale jet of the radio galaxy 3C 390.3