  In this work, we investigate the dynamical effects of a sequence of close
encounters over 200 Myr varying in the interval of 10000 -- 100000 au between a
binary star system and passing stars with masses ranging from 0.1$M_{\odot}$ to
10$M_{\odot}$. We focus on binaries consisting of two Sun-like stars with
various orbital separations $a_{\scriptscriptstyle 0}$ from 50 au to 200 au
initially on circular-planar orbits. We treat the problem statistically since
each sequence is cloned 1000 times. Our study shows that orbits of binaries
initially at $a_{\scriptscriptstyle 0}$ = 50 au will slightly be perturbed by
each close encounter and exhibit a small deviation in eccentricity (+0.03) and
in periapsis distance (+1 and -2 au) around the mean value. However increasing
$a_{\scriptscriptstyle 0}$ will drastically increase these variances: up to
+0.45 in eccentricity and between +63 au and -106 au in periapsis, leading to a
higher rate of disrupted binaries up to 50% after the sequence of close
encounters. Even though the secondary star can remain bound to the primary,
$\sim$20% of the final orbits will have inclinations greater than 10$^{\circ}$.
As planetary formation already takes place when stars are still members of
their birth cluster, we show that the variances in eccentricity and periapsis
distance of Jupiter- and Saturn-like planets will inversely decrease with
$a_{\scriptscriptstyle 0}$ after successive fly-bys. This leads to higher
ejection rate at $a_{\scriptscriptstyle 0}$ = 50 au but to a higher extent for
Saturn-likes (60%) as those planets' apoapsis distances cross the critical
stability distance for such binary separation.
