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We investigate roles of magnetic activity in the Galactic bulge region indriving large-scale outflows of size $\sim 10$ kpc. Magnetic buoyancy andbreakups of channel flows formed by magnetorotational instability excitePoynting flux by the magnetic tension force. A three-dimensional globalnumerical simulation shows that the average luminosity of such \AlfvenicPoynting flux is $10^{40} - 10^{41}$ erg s$^{-1}$. We examine the energy andmomentum transfer from the Poynting flux to the gas by solving time-dependenthydrodynamical simulations with explicitly taking into account low-frequency\Alfvenic waves of period of 0.5 Myr in a one-dimensional vertical magneticflux tube. The \Alfvenic waves propagate upward into the Galactic halo, andthey are damped through the propagation along meandering magnetic field lines.If the turbulence is nearly trans-Alfv\'{e}nic, the wave damping issignificant, which leads to the formation of an upward propagating shock wave.At the shock front, the temperature $\gtrsim 5\times 10^6$ K, the density$\approx 6\times 10^{-4}$ cm$^{-3}$, and the outflow velocity $\approx 400-500$km s$^{-1}$ at a height $\approx 10$ kpc, which reasonably explain the basicphysical properties of the thermal component of the Fermi bubbles.

Galactic Outflows by Alfv\'enic Poynting Flux: Application to Fermi Bubbles