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We present simulations of the evolution of self-gravitating dense gas onkiloparsec-size scales in a galactic disk, designed to study dense clumpformation from giant molecular clouds (GMCs). These dense clumps are expectedto be the precursors to star clusters and this process may be the rate limitingstep controling star formation rates in galactic systems as described by theKennicutt-Schmidt relation. The evolution of these simulated GMCs and clumps isdetermined by self-gravity balanced by turbulent pressure support and the largescale galactic shear. While the cloud structures and densities significantlychange during their evolution, they remain roughly in virial equilibrium fortime scales exceeding the free-fall time of GMCs, indicating that energy fromthe galactic shear continuously cascades down. We implement star formation at aslow, inefficient rate of 2% per local free-fall time, but this yields globalstar formation rates that are more than ~two orders of magnitude larger thanthe observed Kennicutt-Schmidt relation due to the over-production of denseclump gas. To explain this discrepancy, we anticipate magnetic fields toprovide additional support. Low-resolution simulations indeed show that themagnetic field reduces the star formation rate.

Kiloparsec-Scale Simulations of Magnetised Molecular Clouds in Disk Galaxies