  Recent observations of supernovae (SNe) have indicated that a fraction of
massive stars possess dense circumstellar medium (CSM) at the moment of their
core collapses. They suggest the presence of additional activities of the SN
progenitor driving the enhancement of the mass-loss rate, and some physical
processes attributing to single star's activities have been considered. In this
study, we carry out binary evolutionary simulations of massive stars with the
aim of investigating the CSM structure. We show that the mass-transfer rate in
a binary can increase at the beginning of the Roche lobe overflow, and this
enhancement would be associated with the structure of the CSM before the
explosion. We also illustrate that depending on the orbital period of the
binary, the density structure of the CSM can have a diverse distribution
including shell-like and cliff-like structures. These characteristic structures
appear within the lengthscale of $\sim 10^{17}\,{\rm cm}$ and could be traced
by long-term observations of SNe, if the slow velocity of the CSM is assumed
($\sim 10\,{\rm km}\,{\rm s}^{-1}$). Our results highlight the importance of
binary interaction in the aspect of reproducing the diversity of the CSM
configuration.
