  We present the results of high resolution VLBI observations at 1.6 and 4.9
GHz of the radio-loud Seyfert galaxy, Mrk 6. These observations are able to
detect a compact radio core in this galaxy for the first time. The core has an
inverted spectral index ($\alpha^{1.6}_{4.9}$=+1.0$\pm$0.2) and a brightness
temperature of $1\times10^8$ K. Three distinct radio components which resemble
jet elements and/or hot spots, are also detected. The position angles of these
elongated jet elements point, not only to a curved jet in Mrk 6, but also
towards a connection between the AGN and the kpc-scale radio lobes/bubbles in
this galaxy. Firmer constraints on the star formation rate provided by new
Herschel observations (SFR $<0.8$ M$_\sun$ yr$^{-1}$) make the starburst-wind
powered bubble scenario implausible. From plasma speeds obtained via prior
Chandra X-ray observations, and ram pressure balance arguments for the ISM and
radio bubbles, the north-south bubbles are expected to take $7.5\times10^6$ yr
to form, and the east-west bubbles $1.4\times10^6$ yr. We suggest that the jet
axis has changed at least once in Mrk 6 within the last $\approx10^7$ yr. A
comparison of the nuclear radio-loudness of Mrk 6 and a small sample of Seyfert
galaxies with a subset of low-luminosity FRI radio galaxies reveals a continuum
in radio properties.
