Tidal Effects in Clusters of Galaxies

High-redshift clusters of galaxies show an overabundance of spirals by a factor of 2-3 and the corresponding underabundance of S0 galaxies, relative to the nearby clusters. This morphological evolution can be explained by tidal interactions with neighboring galaxies and with the hierarchically growing cluster halo. The efficiency of tidal interactions depends on the size and structure of the cluster, as well as on the epoch of its formation. I simulate the formation and evolution of Virgo-type clusters in three cosmologies: a critical density model Ω₀=1, an open model Ω₀=0.4, and a flat model Ω₀=0.4 with a cosmological constant. The orbits of identified halos are traced with a high temporal resolution (~10⁷ yr). Halos with low relative velocities merge only shortly after entering the cluster; after virialization mergers are suppressed. The dynamical evolution of galaxies is determined by the tidal field along their trajectories. The maxima of the tidal force do not always correspond to closest approach to the cluster center. They are produced to a large extent by the local density structures, such as the massive galaxies and the unvirialized remnants of infalling groups of galaxies. Collisions of galaxies are intensified by the substructure, with about 10 encounters within 10 kpc per galaxy in the Hubble time. These very close encounters add an important amount (10%-50%) of the total heating rate. The integrated effect of tidal interactions is insufficient to transform a spiral galaxy into an elliptical but can produce an S0 galaxy. Overall, tidal heating is stronger in the low-Ω₀ clusters.