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Within Rotation Curves (RC) is encoded the kinematical state of the stellardisc as well as information about the dynamical mechanisms driving the secularevolution of galaxies. To explain the characteristic features of RCs that ariseby the influence of spiral patterns and bar, we study the kinematics of thestellar disc in a set of spiral galaxy models specifically tailored for thispurpose. We find that, for our models, the induced non-circular motions aremore prominent for spirals with larger pitch angle, the ones typical in latetype galaxies. Moreover, inside corotation, stars rotate slower along thespiral arms than along the inter-arm, which translates into a local minima ormaxima in the RC, respectively. We also see, from off-plane RC, that therotation is faster for stars that at observed closer to the plane, anddiminishes as one looks farther off plane; this trend is more noticeable in ourSa galaxy model than our Sc galaxy model. Additionally, in a previous work wefound that the diagonal ridges in the $V_{\phi}-R$ plane, revealed through theGaia DR2, have a resonant origin due to the spiral arms and bar and that theseridges project themselves as wiggles in the RC; here, we further notice thatthe development of these ridges, and the development of high orbitaleccentricities in the stellar disc are the same. Hence, we conclude that, thefollowing explanations of bumps and wiggles in RCs are equivalent: they aremanifestations of diagonal ridges in the $V_{\phi}-R$ plane, or of therearrangement of the orbital eccentricities in the stellar disc.

The imprint of arms and bars on rotation curves: in-plane and off-plane