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The Galactic bar plays a critical role in the evolution of the Milky Way'sCentral Molecular Zone (CMZ), driving mass inward toward the Galactic Centervia gas flows known as dust lanes. To explore the interaction between the CMZand the dust lanes, we run hydrodynamic simulations in AREPO, modeling thepotential of the Milky Way's bar in the absence of gas self-gravity and starformation physics, and we study the flows of mass using Monte Carlo tracerparticles. We estimate the efficiency of the inflow via the dust lanes, findingthat only about a third (30$\pm$12%) of the dust lanes' mass initially accretesonto the CMZ, while the rest overshoots and accretes later. Given observationalestimates of the amount of gas within the Milky Way's dust lanes, this suggeststhat the true total inflow rate onto the CMZ is 0.8$\pm$0.6M$_\odot$~yr$^{-1}$. Clouds in this simulated CMZ have sudden peaks in theiraverage density near the apocenter, where they undergo violent collisions withinflowing material. While these clouds tend to counter-rotate due to shear,co-rotating clouds occasionally occur due to the injection of momentum fromcollisions with inflowing material (~52% are strongly counter-rotating, and ~7%are strongly co-rotating of the 44 cloud sample). We investigate the formationand evolution of these clouds, finding that they are fed by many discreteinflow events, providing a consistent source of gas to CMZ clouds even as theycollapse and form stars

Dynamically Driven Inflow onto the Galactic Center and its Effect upon Molecular Clouds