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By performing a global magneto-hydrodynamical simulation for the Milky Waywith an axisymmetric gravitational potential, we propose that spatiallydependent amplification of magnetic fields possibly explains the observednoncircular motion of the gas in the Galactic center region. The radialdistribution of the rotation frequency in the bulge region is not monotonic ingeneral. The amplification of the magnetic field is enhanced in regions withstronger differential rotation, because magnetorotational instability andfield-line stretching are more effective. The strength of the amplifiedmagnetic field reaches >~ 0.5 mG, and radial flows of the gas are excited bythe inhomogeneous transport of angular momentum through turbulent magneticfield that is amplified in a spatially dependent manner. In addition, themagnetic pressure-gradient force also drives radial flows in a similar manner.As a result, the simulated position-velocity diagram exhibits a time-dependentasymmetric parallelogram-shape owing to the intermittency of the magneticturbulence; the present model provides a viable alternative to thebar-potential-driven model for the parallelogram-shape of the central molecularzone. This is a natural extension into the central few 100 pc of the magneticactivity, which is observed as molecular loops at radii from a few 100 pc to 1kpc. Furthermore, the time-averaged net gas flow is directed outward, whereasthe flows are highly time-dependent, which we discuss from a viewpoint of theoutflow from the bulge.

Stochastic Noncircular Motion and Outflows Driven by Magnetic Activity in the Galactic Bulge Region