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We present three high resolution radio images of the Crab nebula, taken in 1998.6, 1998.8 and 2000.1 with the VLA. These are the best radio images of the Crab to date. We show that, near the pulsar, there are significant changes between our three observing epochs. These changes have an elliptical geometry very similar to that of the optical wisps. One radio wisp in particular can be unambiguously identified between two of our observing epochs, and moves outward with an apparent velocity of ~0.24. The similarity in both morphology and behavior of the present radio wisps to the optical wisps suggests that they are associated. This implies that the radio wisps, like the optical ones, are likely manifestations of the shock in the Crab pulsar's wind. This suggests that the radio emitting electrons are accelerated in the same region as the ones responsible for the optical to X-ray emission, contrary to most current models., Comment: 12 pages, 5 figures (6 figure files), LaTeX, accepted for publication in the Astrophysical Journal

In the best established of apparently superrelativistic radio source expansion velocities, that of 3C 345, the reported apparent velocity of approx.2.5c is reduced to one of approx.0.1c in the chronometric cosmology. All other published apparent superrelativistic velocities are also reduced to subrelativistic levels.

Observations of 3C 395, obtained at 4.990 GHz with an eight-station VLBI on June 1, 1985 and at 1.66 GHz using a similar seven-station network in late 1984, are reported. The data are presented in tables and maps along with the observations from 1979 (Johnston et al., 1983) and 1983 (Waak et al., 1985) and discussed in detail. Three compact-structure components are identified as (1) the central core, which became 0.4 Jy brighter between 1983 and 1985, (2) a stationary secondary component with nearly constant flux density, and (3) a constant-flux-density component moving from (1) to (2) at 0.64 + or - 0.1 marcsec/yr, corresponding to apparent velocity 15/h x c for H0 = 100h km/s Mpc and q0 = 0.05. 21 references.

interferometer observations made during two years with the Goldstack interferometer show considerable increases and decreases in the apparent angular size of the radio galaxy 3C 120. The data suggest that the outbursts occur in regions separated by several light years but are also consistent with the individual components expanding or moving with an apparent velocity close to the speed of light.