  We study the three-dimensional evolution of a viscous protoplanetary disc
which accretes gas material from a second protoplanetary disc during a close
encounter in an embedded star cluster. The aim is to investigate the capability
of the mass accretion scenario to generate strongly inclined gaseous discs
which could later form misaligned planets. We use smoothed particle
hydrodynamics to study mass transfer and disc inclination for passing stars and
circumstellar discs with different masses. We explore different orbital
configurations to find the parameter space which allows significant disc
inclination generation.
  \citet{Thi2011} suggested that significant disc inclination and disc or
planetary system shrinkage can generally be produced by the accretion of
external gas material with a different angular momentum. We found that this
condition can be fullfilled for a large range of gas mass and angular momentum.
  For all encounters, mass accretion from the secondary disc increases with
decreasing mass of the secondary proto-star. Thus, higher disc inclinations can
be attained for lower secondary stellar masses. Variations of the secondary
disc's orientation relative to the orbital plane can alter the disc evolution
significantly.
  The results taken together show that mass accretion can change the
three-dimensional disc orientation significantly resulting in strongly inclined
discs. In combination with the gravitational interaction between the two
star-disc systems, this scenario is relevant for explaining the formation of
highly inclined discs which could later form misaligned planets.
