Dynamical Models of the Barred Spiral Galaxy NGC 3992

In this paper we construct dynamical models that partially reproduce observations of H I in the barred spiral galaxy NGC 3992. The models are constrained by the large-scale structure and kinematics of the gas (Paper I) and by the near-infrared morphology of the bar. The dynamical components we have considered consist of (1) an axisymmetric Toomre disk of index n=0, truncated as indicated in Paper I; (2) a triaxial stellar bar constrained by near-infrared photometry; (3) an oval distortion of the axisymmetric disk; and (4) a spherical halo constrained by the observed kinematics and truncation of the disk (Paper I).