  The NASA K2 mission that succeeded the nominal Kepler mission observed
several hundreds of thousands of stars during its operations. While most of the
stars were observed in single campaigns of 80 days, some of them were targeted
for more than one campaign. We perform an asteroseismic study of a sample of
eight solar-like stars observed during K2 Campaigns 6 and 17. We first extract
the light curves for the two campaigns using two different pipelines, EVEREST
and Lightkurve. The seismic analysis is done on the combined light curve of C6
and C17 where the gap between them was removed and the two campaigns were
stitched together. We determine the global seismic parameters of the solar-like
oscillations using two different methods (A2Z pipeline and the apollinaire
code). We perform the peak-bagging of the modes to characterize their
individual frequencies. By combining the frequencies with the Gaia DR2
effective temperature and luminosity, and metallicity for five of the targets,
we determine the fundamental parameters of the targets using the IACgrids based
on the MESA code. While the masses and radii of our targets probe a similar
parameter space compared to the Kepler solar-like stars with detailed modeling,
we find that for a given mass our more evolved stars seem to be older compared
to previous seismic stellar ensembles. We calculate the stellar parameters
using two different grids of models, incorporating and excluding the treatment
of diffusion, and find that the results agree generally within the
uncertainties, except for the ages. The seismic radii and the Gaia DR2 radii
present an average difference of 4% with a dispersion of 5%. Although the
agreement is quite good, the seismic radii are slightly underestimated compared
to Gaia DR2 for our stars, the disagreement being greater for the more evolved
ones.
