2019MNRAS.485L.116S

The period-mass and period-radius distributions of exoplanets are known to exhibit a desert. Unlike the existence of very hot (P_orb < 3 d) super-Earths and hot Jupiters, no planets are known between super-Earths and sub-Jupiters with orbital periods as short as a day or two. In this letter, we show that the period boundary of this desert is dependent on stellar parameters (T_eff, [M/H], log g in order of significance), there is conclusive dependence on the incident stellar irradiation, and dependence on the stellar mass acting only on planets around T_eff < 5600 K host stars. We found a significant lack of very inflated planets on the closest orbits to the host star. There is no significant dependence on tidal forces currently acting on the planet, the planet's surface gravity, or current filling factor of the Roche lobe. These distributions are most compatible with the dominant role of photoevaporation in forming the desert.