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The highly-substructured outskirts of the Magellanic Clouds provide ideallocations for studying the complex interaction history between both Clouds andthe Milky Way (MW). In this paper, we investigate the origin of a >20$^\circ$long arm-like feature in the northern outskirts of the Large Magellanic Cloud(LMC) using data from the Magellanic Edges Survey (MagES) and Gaia EDR3. Wefind that the arm has a similar geometry and metallicity to the nearby outerLMC disk, indicating that it is comprised of perturbed disk material. Whilstthe azimuthal velocity and velocity dispersions along the arm are consistentwith those in the outer LMC, the in-plane radial velocity and out-of-planevertical velocity are significantly perturbed from equilibrium disk kinematics.We compare these observations to a new suite of dynamical models of theMagellanic/MW system, which describe the LMC as a collection of tracerparticles within a rigid potential, and the SMC as a rigid Hernquist potential.Our models indicate the tidal force of the MW during the LMC's infall is likelyresponsible for the observed increasing out-of-plane velocity along the arm.Our models also suggest close LMC/SMC interactions within the past Gyr,particularly the SMC's pericentric passage ~150 Myr ago and a possible SMCcrossing of the LMC disk plane ~400 Myr ago, likely do not perturb stars thattoday comprise the arm. Historical interactions with the SMC prior to ~1 Gyrago may be required to explain some of the observed kinematic properties of thearm, in particular its strongly negative in-plane radial velocity.

The Magellanic Edges Survey -- II. Formation of the LMC's northern arm