Hydro and Magnetohydrodynamics of the Galactic Gas Spiral Pattern

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Better data over the past few years permit now a more refined modeling of Galactic mass distributions in the bar and spiral components. Coupling self-consistently in the dynamic sense (stellar orbital response in phase with the spiral perturbation) a stellar spiral pattern guided by observations with the other Galactic components -- dark halo, disk and bulge, a large scale 3D gas response can be numerically studied with the ZEUS MP code. First, a difference that is commonly observed in galaxies, that the K band image of a 2 armed spiral contrasts with an optical 4 armed pattern, is obtained as the hydro (and MHD) response to a 2 stellar pattern with gas orbiting in a full Galactic mass distribution model. For that, the angular speed of the stellar spiral pattern Vp must exceed a certain threshold value. Values lesser than Vp don't produce a 4 arms pattern and the 2 armed gaseous pattern coincides with the imposed 2 armed stellar pattern. In the presence of a circular or spiral magnetic field, the response can give rise to an instability which produces large scale turbulence and has a strong impact on the structure of the gaseous disk, preserving the large scale quasi-stationary spiral gas pattern.

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