Abstract
We present self-consistent numerical simulations of the molecular gas in the spiral galaxy NGC 3359. Using the real potential derived from an I-band image, we have tried to find the dynamical parameters able to account for the observed gas kinematics and morphology (in both Ha and HI). The best result is obtained for a two pattern speeds model: the central region (up to ~ 15”), corresponding to a nuclear bar, rotates with an Ω p = 100 km s-1 kpc -1.The outer bar+spiral, decoupled from the nuclear region, has a slower angular velocity Ω p = 27 km s-1 kpc -1. The model reproduces the complex Hα structure in the inner 20” radius, which is certainly not fitted with the one mode pattern.
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