1996A&A...308..415B

We present third epoch VLBI observations at 1.67GHz of a sample of 20 Low Frequency Variable Sources. The sources have been observed with a global array of 11 radio telescopes, recording in MK 2 mode, with a resolution of ∼3mas. We also present an analysis of possible variations in the fringe visibilities between an earlier epoch (1981.8) and the present epoch (1987.9), and compare these changes with those observed between the two epochs 1980.1 and 1981.8. Significant variations have been found in 17 out of 20 sources. In a number of cases the changes are clearly due to flux density variations in the most compact component. Several other cases appear to be due to either an increase in the angular size of a single component or a change in the angular separation between well defined components. Some sources show superluminal motions much like those usually observed at higher frequencies, and some new candidates for superluminal motions are identified. We have also used 408MHz monitoring data, taken in the period of the VLBI observations, to derive an estimate of the Doppler factors necessary to account for the low frequency variability, and we compare these values with the Doppler factors calculated from the proper motions detected in our VLBI observations. This analysis confirms that two distinct phenomena, intrinsic superluminal beaming and extrinsic scintillation, are responsible for the low frequency variability seen in compact extragalactic radio sources.