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A pair of non-thermal radio bubbles recently discovered in the inner fewhundred parsecs of the Galactic center bears a close spatial association withelongated, thermal X-ray features called the X-ray chimneys. While theirmorphology, position, and orientation vividly point to an outflow from theGalactic center, the physical processes responsible for the outflow remain tobe understood. We use three-dimensional magnetohydrodynamic simulations to testthe hypothesis that the radio bubbles/X-ray chimneys are the manifestation ofan energetic outflow driven by multiple core-collapsed supernovae in thenuclear stellar disk, where numerous massive stars are known to be present. Oursimulations are run with different combinations of two main parameters, thesupernova birth rate and the strength of a global magnetic field beingvertically oriented with respect to the disk. The simulation results show thata hot gas outflow can naturally form and acquire a vertically elongated shapedue to collimation by the magnetic pressure. In particular, the simulation withan initial magnetic field strength of 80 $\mu$G and a supernova rate of 1$kyr^{-1}$ can well reproduce the observed morphology, internal energy andX-ray luminosity of the bubbles after an evolutionary time of 330 kyr. On theother hand, a magnetic field strength of 200 $\mu$G gives rise to an overlyelongated outflow that is inconsistent with the observed bubbles. Thesimulations also reveal that, inside the bubbles, mutual collisions between theshock waves of individual supernovae produce dense filaments of locallyamplified magnetic field. Such filaments may account for a fraction of thesynchrotron-emitting radio filaments known to exist in the Galactic center.

A Supernova-driven, Magnetically-collimated Outflow as the Origin of the Galactic Center Radio Bubbles