  The increasing number of super-Earths close to their host stars revealed a
scarcity of close-in small planets with 1.5-2.0$\,R_\oplus$ in the radius
distribution of ${\it Kepler}$ planets. The atmospheric escape of super-Earths
by photoevaporation can explain the origin of the observed "radius gap." Many
theoretical studies considered the in-situ mass loss of a close-in planet.
Planets that undergo the atmospheric escape, however, move outward due to the
change in the orbital angular momentum of their star-planet systems. In this
study, we calculate the orbital evolution of an evaporating super-Earth with a
H$_2$/He atmosphere around FGKM-type stars under a stellar X-ray and extreme UV
irradiation (XUV). The rate of increase in the orbital radius of an evaporating
planet is approximately proportional to that of the atmospheric mass loss
during a high stellar XUV phase. We show that super-Earths with a rocky core of
$\lesssim$ 10$\,M_\oplus$ and a H$_2$/He atmosphere at $\lesssim$
0.03-0.1$\,$au ($\lesssim$ 0.01-0.03$\,$au) around G-type stars (M-type stars)
are prone to the outward migration driven by photoevaporation. Although the
changes in the orbits of the planets would be small, they would rearrange the
orbital configurations of compact, multi-planet systems, such as the TRAPPIST-1
system. We also find that the radius gap and the so-called "Neptune desert" in
the observed population of close-in planets around FGK-type stars still appear
in our simulations. On the other hand, the observed planet population around
M-type stars can be reproduced only by a high stellar XUV luminosity model.
