  We present a study of the parsec-scale multi-frequency properties of the
quasar S4 1030+61 during a prolonged radio and gamma-ray activity. Observations
were performed within Fermi gamma-ray telescope, OVRO 40-m telescope and MOJAVE
VLBA monitoring programs, covering five years from 2009. The data are
supplemented by four-epoch VLBA observations at 5, 8, 15, 24, and 43 GHz, which
were triggered by the bright gamma-ray flare, registered in the quasar in 2010.
The S4 1030+61 jet exhibits an apparent superluminal velocity of (6.4+-0.4)c
and does not show ejections of new components in the observed period, while
decomposition of the radio light curve reveals nine prominent flares. The
measured variability parameters of the source show values typical for
Fermi-detected quasars. Combined analysis of radio and gamma-ray emission
implies a spatial separation between emitting regions at these bands of about
12 pc and locates the gamma-ray emission within a parsec from the central
engine. We detected changes in the value and direction of the linear
polarization and the Faraday rotation measure. The value of the intrinsic
brightness temperature of the core is above the equipartition state, while its
value as a function of distance from the core is well approximated by the
power-law. Altogether these results show that the radio flaring activity of the
quasar is accompanied by injection of relativistic particles and energy losses
at the jet base, while S4 1030+61 has a stable, straight jet well described by
standard conical jet theories.
