  Although several S-type and P-type planets in binary systems were discovered
in past years, S-type planets have not yet been found in close binaries with an
orbital separation not more than 5 au. Recent studies suggest that S-type
planets in close binaries may be detected through high-accuracy observations.
However, nowadays planet formation theories imply that it is difficult for
S-type planets in close binaries systems to form in situ. In this work, we
extensively perform numerical simulations to explore scenarios of planet-planet
scattering among circumbinary planets and subsequent tidal capture in various
binary configurations, to examine whether the mechanism can play a part in
producing such kind of planets. Our results show that this mechanism is robust.
The maximum capture probability is $\sim 10\%$, which can be comparable to the
tidal capture probability of hot Jupiters in single star systems. The capture
probability is related to binary configurations, where a smaller eccentricity
or a low mass ratio of the binary will lead to a larger probability of capture,
and vice versa. Furthermore, we find that S-type planets with retrograde orbits
can be naturally produced via capture process. These planets on retrograde
orbits can help us distinguish in situ formation and post-capture origin for
S-type planet in close binaries systems. The forthcoming missions (PLATO) will
provide the opportunity and feasibility to detect such planets. Our work
provides several suggestions for selecting target binaries in search for S-type
planets in the near future.
