  The distribution of dark matter (DM) inside galaxies is not uniform. Near the
central regions, its density is the highest. Then, it is logical to suppose
that, inside galaxies, DM affects the physics of stars in central regions more
than outer regions. Besides, current stellar evolutionary models did not
consider DM effects in their assumptions. To consider the DM effects, at first
one must estimate how much DM a star contains. The capture rate (CR) of DM
particles by individual stars was investigated already in the literature. In
this work, we discuss how CR can be affected when stars are members of binary
star systems (BSS) (instead of studying them individually). When a star is a
member of a BSS, its speed changes periodically due to the elliptical motion
around its companion star. In this work, we investigated CR by BSSs in
different BSS configurations. In the end, we discussed observational signatures
that can be attributed to the DM effects in BSSs.
