2025MNRAS.542.2877U

Spherical galaxy models with radially anisotropic velocity distributions merge faster than their isotropic counterparts. Here, we investigate the effects of radially anisotropic haloes on the dynamics of disc galaxy encounters. We use stable galaxy models with isotropic bulges, thin rotating discs and dark haloes which are either isotropic or radially anisotropic. Our simulations confirm that anisotropy can markedly accelerate orbit decay in galaxy interactions; in particular, radially anisotropic haloes transfer a good deal of orbital angular momentum to internal motions even before the galaxies reach their first pericentre. Consequently, for a given initial orbit, the anisotropic models undergo closer and more violent interactions, and their discs generate more massive tidal features. If real disc galaxies have radially anisotropic haloes, our findings may have implications for estimated merger time-scales and remnant morphology.