  The advent of space-based photometry missions such as CoRoT, Kepler and TESS
has sparkled the development of asteroseismology and exoplanetology. The advent
of PLATO will further strengthen such multi-disciplinary studies. Testing
asteroseismic modelling and its importance for our understanding of planetary
systems is crucial. We carried out a detailed modelling of Kepler-93, an
exoplanet host star observed by Kepler. This star is particularly interesting
as it is very similar to the PLATO benchmark target (G spectral type, ~ 6000K,
~ 1 Msun and ~ 1 Rsun) and provides a real-life testbed for potential
procedures to be used for PLATO. We use global and local minimization
techniques for the seismic modelling of Kepler-93, varying the ingredients of
our stellar models. We compute seismic inversions of the mean density. We use
these revised stellar parameters to provide new planetary parameters and
simulate the orbital evolution of the system under the effects of tides and
atmospheric evaporation. Our fundamental parameters for Kepler-93: mean density
= 1.654 +/- 0.004 g/cm3, M = 0.907 +/- 0.023 Msun , R = 0.918 +/- 0.008 Rsun
and Age = 6.78 +/- 0.32 Gyr. The uncertainties we report for this benchmark are
within the requirements of PLATO. For the exoplanet Kepler-93b, we find Mp =
4.01 +/- 0.67 Mearth, Rp = 1.478 +/- 0.014 Rearth and semi-major axis a =
0.0533 +/- 0.0005 AU. According to our simulations, it seems unlikely that
Kepler-93b formed with a mass large enough to be impacted by stellar tides. For
the benchmark of PLATO, detailed asteroseismic modelling procedures will be
able to provide fundamental stellar parameters within the requirements. We
illustrate what synergies can be achieved regarding the orbital evolution and
atmospheric evaporation of exoplanets. We note the importance of the
high-quality radial velocity follow-up to constrain the formation scenarii of
exoplanets.
