Abstract
The gravitational interaction between the Large Magellanic Cloud (LMC) and the Small Magellanic Cloud is evident when GaiaDR3 reveals the shape of the Magellanic bridge in the young stellar evolutionary phase and the velocity flow also in older and evolved populations. The imprint of the interaction in the LMC in-plane velocity field is not clear. The radial velocity field in the outer parts of the disc of the LMC is not consistent with a disc in equilibrium. We plan to use the KRATOS simulations, a suite of 24 LMC-like N-body simulations, to analyse the effect of the SMC on the LMC disc kinematics.