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In current models for jets of AGNs and their emission a shortcoming in thedescription and understanding of the connection between the largest andsmallest scales exists. In this work we present a spatially resolved SSC modelextended to parsec scales, which opens the possibility of probing theconnections between the radio and high energy properties. We simulate anenvironment that leads to Fermi-I acceleration of leptonic particles andincludes the full time dependence of this process. Omitting the restriction ofa finite downstream region, we find that the spectral energy distribution (SED)produced by the accelerated particles strongly depends on their radialconfinement behind the shock. The requirement, for both the restriction of highenergy emission to a small region around the shock and the production of a flatradio spectrum, is an initial linear increase of the radius immediately behindthe shock, which then slows down with increasing distance from the shock. Agood representation of the data for the Blazar \textit{Mkn501} is achieved by aparameterized log-function. The prediction for the shape of the radio blob isgiven by the flux distribution with respect to shock distance.

A numerical model of parsec scale SSC morphologies and their radio emission