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We study the three-dimensional evolution of a viscous protoplanetary discwhich accretes gas material from a second protoplanetary disc during a closeencounter in an embedded star cluster. The aim is to investigate the capabilityof the mass accretion scenario to generate strongly inclined gaseous discswhich could later form misaligned planets. We use smoothed particlehydrodynamics to study mass transfer and disc inclination for passing stars andcircumstellar discs with different masses. We explore different orbitalconfigurations to find the parameter space which allows significant discinclination generation.  \citet{Thi2011} suggested that significant disc inclination and disc orplanetary system shrinkage can generally be produced by the accretion ofexternal gas material with a different angular momentum. We found that thiscondition can be fullfilled for a large range of gas mass and angular momentum.  For all encounters, mass accretion from the secondary disc increases withdecreasing mass of the secondary proto-star. Thus, higher disc inclinations canbe attained for lower secondary stellar masses. Variations of the secondarydisc's orientation relative to the orbital plane can alter the disc evolutionsignificantly.  The results taken together show that mass accretion can change thethree-dimensional disc orientation significantly resulting in strongly inclineddiscs. In combination with the gravitational interaction between the twostar-disc systems, this scenario is relevant for explaining the formation ofhighly inclined discs which could later form misaligned planets.

Generation of inclined protoplanetary discs and misaligned planets through mass accretion I: Coplanar secondary discs