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We show that collisions between the outer Galactic HI disk and the leadingarms (LAs) of the Magellanic stream (MS) can create giant HI holes andchimney-like structures in the disk. Based on the results of our N-bodysimulations on the last 2.5 Gyr evolution of the Large and Small MagellanicClouds (LMC and SMC, respectively) interacting with the Galaxy, we investigatewhen and where the LAs can pass through the Galactic plane after the MSformation. We then investigate hydrodynamical interaction between LAs and theGalactic HI disk (``the Magellanic impact'') by using our new hydrodynamicalsimulations with somewhat idealized models of the LAs. We find that about 1-3%of the initial gas mass of the SMC, which consists of the LAs, can pass throughthe outer part (R=20-35 kpc) of the Galactic HI disk about 0.2 Gyr ago. We alsofind that the Magellanic impact can push out some fraction (~1%) of the outerGalactic HI disk to form 1-10 kpc-scale HI holes and chimney-like bridgesbetween the LAs and the disk.

The Magellanic impact: Collision between the outer Galactic HI disk and the leading arms of the Magellanic stream