One-Armed Spiral Waves in Galaxy Simulations with Counter-Rotating Stars One-Armed Spiral Waves in Galaxy Simulations with Counter-Rotating Stars

Motivated by observations of disk galaxies with counter-rotating stars, we have run two-dimensional, collisionless N−body simulations of disk galaxies with significant counter-rotating components. For all our simulations the initial value of Toomre’s stability parameter was Q = 1.1. The percentage of counter-rotating particles ranges from 25% to 50%. A stationary one-arm spiral wave is observed to form in each run, persisting from a few to five rotation periods, measured at the half-mass radius. In one run, the spiral wave was initially a leading arm which subsequently transformed into a trailing arm. We also observed a change in spiral direction in the run initially containing equal numbers of particles orbiting in both directions. The results of our simulations support an interpretation of the one armed waves as due to the two stream instability. Subject headings: gravitation—instabilities—galaxies: evolution—kinematics & dynamics—stars:kinematics