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NGC 6782 is an early-type barred spiral galaxy exhibiting a rich and complexmorphology with multiple ring patterns. To provide a physical understanding ofits structure and kinematical properties, two-dimensional hydrodynamicalsimulations have been carried out. Numerical calculations reveal that thestriking features in NGC 6782 can be reproduced provided that the gas flow isgoverned by the gravitational potential associated with a slowly rotatingstrong bar. In particular, the response of the gaseous disk to the barpotential leads to the excitation of spiral density waves at the inner Lindbladresonance giving rise to the appearance of a nearly circular nuclear ring witha pair of dust lanes. For a sufficiently strong bar potential, the inner 4:1spiral density waves are also excited. The interaction of the higher harmonicwaves with the waves excited at the inner Lindblad resonance and confined bythe outer Lindblad resonance results in the observed diamond-shaped (or pointyoval) inner ring structure. The overall gas morphology and kinematical featuresare both well reproduced by the model provided that the pattern speed of thebar is $\sim 25$ km s$^{-1}$ kpc$^{-1}$.

Hydrodynamical Simulations of the Barred Spiral Galaxy NGC 6782