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We have run fully self-consistent stellar dynamical simulations of the accretion of a small galaxy by a large disk galaxy and found that an X-shaped structure forms in the disk after the merger is complete. We wish to emphasize that this structure consists mostly of disk material rather than accreted material. The result is morphologically similar to such peculiar S0 galaxies as NGC~128, NGC~7332, Hickson~87A, and IC~4767, an assertion quantitatively supported by the ``$a_4$'' ($\cos 4 \theta$) coefficient. A possible evolutionary link between spiral and S0 galaxies is suggested.
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