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Tidal interactions between disc galaxies and low mass companions are anestablished method for generating galactic spiral features. In this work wepresent a study of the structure and dynamics of spiral arms driven ininteractions between disc galaxies and perturbing companions in 3-DN-body/smoothed hydrodynamical numerical simulations. Our specific aims are tocharacterize any differences between structures formed in the gas and starsfrom a purely hydrodynamical and gravitational perspective, and to find alimiting case for spiral structure generation. Through analysis of a number ofdifferent interacting cases, we find that there is very little differencebetween arm morphology, pitch angles and pattern speeds between the two media.The main differences are a minor offset between gas and stellar arms, clearspurring features in gaseous arms, and different radial migration of materialin the stronger interacting cases. We investigate the minimum mass of acompanion required to drive spiral structure in a galactic disc, finding thelimiting spiral generation cases with companion masses of the order$1\times10^9M_\odot$, equivalent to only 4% of the stellar disc mass, or 0.5%of the total galactic mass of a Milky Way analogue.

Gas and stellar spiral structures in tidally perturbed disc galaxies