  Asteroseismology has been impressively boosted during the last decade mainly
thanks to space missions such as Kepler/K2 and CoRoT. This has a large impact,
in particular, in exoplanetary sciences since the accurate characterization of
the exoplanets is convoluted in most cases with the characterization of their
hosting star. Until the expected launch of the ESA mission PLATO 2.0, there is
almost a decade where only two important missions will provide short-cadence
high-precision photometric time-series: NASA--TESS and ESA--CHEOPS missions,
both having high capabilities for exoplanetary sciences. In this work, we want
to explore the asteroseismic potential of CHEOPS time-series. Following the
works done for estimating the asteroseismic potential of Kepler and TESS, we
have analyzed the probability of detecting solar-like pulsations using CHEOPS
light-curves. Since CHEOPS will collect runs with observational times from
hours up to a few days, we have analyzed the accuracy and precision we can
obtain for the estimation of nu_max, the only asteroseismic observable we can
recover using CHEOPS observations. Finally, we have analyzed the impact of
knowing nu_max in the characterization of exoplanet host stars. Using CHEOPS
light-curves with the expected observational times we can determine nu_max for
massive G and F-type stars from late Main Sequence on, and for F, G, and K-type
stars from post-Main Sequence on with an uncertainty lower than a 5%. For
magnitudes V<12 and observational times from eight hours up to two days, the HR
zone of potential detectability changes. The determination of nu_max leads to
an internal age uncertainty reduction in the characterization of exoplanet host
stars from 52% to 38%; mass uncertainty reduction from 2.1% to 1.8%; radius
uncertainty reduction from 1.8% to 1.6%; density uncertainty reduction from
5.6% to 4.7%, in our best scenarios.
