2006MNRAS.370....2S

Recent ideas for the origin and persistence of the warps commonly observed in disc galaxies have focused on cosmic infall. We present N-body simulations of an idealized form of cosmic infall on to a disc galaxy and obtain a warp that closely resembles those observed. The inner disc tilts remarkably rigidly, indicating strong cohesion due to self-gravity. The line of nodes (LON) of the warp inside R_26.5∼ 4.5R_d is straight, while that beyond R_26.5 generally forms a loosely wound, leading spiral in agreement with Briggs's rules. We focus on the mechanism of the warp and show that the leading spiral arises from the torques from the misaligned inner disc and its associated inner oblate halo. The fact that the LON of most warps forms a leading spiral might imply that the disc mass is significant in the centre. If the LON can be traced to very large radii in future observations, it may reveal information on the mass distribution of the outer halo. The warp is not strongly damped by the halo because the precession rate of the inner disc is slow and the inner halo generally remains aligned with the inner disc. Thus, even after the imposed quadrupolar perturbation is removed, the warp persists for a few Gyr, by which time another infall event can be expected.