  High-velocity atomic clouds in the Galactic center have attracted significant
attention due to their enigmatic formation process, which is potentially linked
to the starburst or supermassive black hole activities in the region. Further,
the discovery of high-velocity molecular clouds (HVMCs) presents a greater
puzzle, because they are much denser and more massive. If the HVMCs were
accelerated by the strong activities in the Galactic center, they are expected
to be destroyed before they reach such a high velocity. To shed light on this
phenomenon, we perform three-dimensional numerical simulations to investigate
the origin and hydrodynamic evolution of HVMCs during a starburst in the
Galactic center. We find that the presence of a magnetic field provides
effective protection and acceleration to molecular clouds (MCs) within the
galactic winds. Consequently, the MCs can attain latitudes of approximately 1
kpc with velocities around 200 km/s, consistent with the observed
characteristics of HVMCs. The consistency of our findings across a wide
parameter space supports the conclusion that HVMCs can indeed withstand the
starburst environment in the Galactic center, providing valuable insights into
their survival mechanisms.
