2024MNRAS.527.3418Z

High-velocity atomic clouds in the Galactic centre 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 centre, they are expected to be destroyed before they reach such a high velocity. To shed light on this phenomenon, we perform 3D numerical simulations to investigate the origin and hydrodynamic evolution of HVMCs during a starburst in the Galactic centre. 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^–1, 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 centre, providing valuable insights into their survival mechanisms.