Abstract
In this work we have determined a dynamical model for NGC 3359. This is a strongly barred spiral galaxy with a complex structure, within which we can see an annular zone of intense star formation. In this work we present self consistent numerical simulations of molecular gas in NGC 3359; and using the potential derived from an I band image, we attempt to find the parameters responsible for the kinematics and morphology of the observed gas. The best results are obtained for a two pattern speed model: the central region (up to 15 arcsec) corresponding to the nuclear bar which rotates with a Ω_{s}=100 km s^{-1} kpc^{-1}; and the main bar + outer spiral, decoupled from the nuclear region, which rotates with a angular velocity, Ω_{p}=27 km s^{-1} kpc^{-1}. The model successfully reproduces the complex structure in Hα of the galaxy in the internal 20 arcsec zone, which cannot really be explained with a unique mode pattern.
