  We investigate the influence of photoevaporation of protoplanetary discs on
the final distribution of exoplanets semi-major axis distances. We model giant
planet migration in viscous discs affected by photoevaporation driven by either
pure EUV or soft X-ray radiation (XEUV). We show that the final exoplanet
distributions are strongly dependant on the choice of the photoevaporation
model. In particular, we find that XEUV is more efficient than pure EUV
radiation at parking planets at approximately 1-2 AU distance from their
central star, hence roughly reproducing the observed peak in the exoplanets
semi-major axis distributions. We note however that a more quantitative
comparison with the observations is hindered by the oversimplified treatment of
planetary accretion, which severely affects migration rates. For this reason,
caution should be used when using these models to constrain details of disc
clearing and/or migration from the observations. Nevertheless our results
indicate that disc dispersal by photoevaporation may be the main driver of the
features in the exoplanets semi-major axis distribution observed by recent
surveys.
