  During their evolution, short-period exoplanets may lose envelope mass
through atmospheric escape owing to intense XUV (X-ray and extreme ultraviolet)
radiation from their host stars. Roche-lobe overflow induced by orbital
evolution or intense atmospheric escape can also contribute to mass loss. To
study the effects of mass loss on inner planet populations, we calculate the
evolution of hot Jupiters considering mass loss of their envelopes and thermal
contraction. Mass loss is assumed to occur through XUV-driven atmospheric
escape and the following Roche-lobe overflow. The runaway effect of mass loss
results in a dichotomy of populations: hot Jupiters that retain their envelopes
and super Earths whose envelopes are completely lost. Evolution primarily
depends on the core masses of planets and only slightly on migration history.
In hot Jupiters with small cores (~10 Earth masses), runaway atmospheric escape
followed by Roche-lobe overflow may create sub-Jupiter deserts, as observed in
both mass and radius distributions of planetary populations. Comparing our
results with formation scenarios and observed exoplanets populations, we
propose that populations of closely orbiting exoplanets are formed by capturing
of planets at/inside the inner edges of protoplanetary disks and subsequent
evaporation of sub-Jupiters.
