  In spring 2005 the blazar 3C 454.3 was observed in an unprecedented bright
state from the near-IR to the hard X-ray frequencies. A mm outburst peaked in
June-July 2005, and it was followed by a flux increase at high radio
frequencies. In this paper we report on multifrequency monitoring by the WEBT
aimed at following the further evolution of the outburst in detail. In
particular, we investigate the expected correlation and time delays between the
optical and radio emissions in order to derive information on the variability
mechanisms and jet structure. A comparison among the light curves at different
frequencies is performed by means of visual inspection and discrete correlation
function, and the results are interpreted with a simple model taking into
account Doppler factor variations of geometric origin. The high-frequency radio
light curves show a huge outburst starting during the dimming phase of the
optical one and lasting more than 1 year. The first phase is characterized by a
slow flux increase, while in early 2006 a major flare is observed. The
lower-frequency radio light curves show a progressively delayed and fainter
event, which disappears below 8 GHz. We suggest that the radio major peak is
not physically connected with the spring 2005 optical one, but it is actually
correlated with a minor optical flare observed in October-November 2005. This
interpretation involves both an intrinsic and a geometric mechanism. The former
is represented by disturbances travelling down the emitting jet, the latter
being due to the curved-jet motion, with the consequent differential changes of
viewing angles of the different emitting regions.
