We compare different dynamical models to study the motion of Trojans. Besides the three dimensional restricted three-and fourbody problem (Jupiter AND Saturn) we also study the motion of the Trojans in the model of the outer Solar system (OSS). Particularly we investigate how the stability zones depend on the inclinations of the Trojans asteroids. Besides straight forward numerical integrations of real AND fictitious Trojans we also use the LCEs as chaos indicators. We find some slight differences in the extension of the stability region for L4 and L5 when we compare the restricted four body problem with the OSS.