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We use simulations with realistic models for stellar feedback to study galaxymergers. These high resolution (1 pc) simulations follow formation anddestruction of individual GMCs and star clusters. The final starburst isdominated by in situ star formation, fueled by gas which flows inwards due toglobal torques. The resulting high gas density results in rapid star formation.The gas is self gravitating, and forms massive (~10^10 M_sun) GMCs andsubsequent super-starclusters (masses up to 10^8 M_sun). However, in contrastto some recent simulations, the bulk of new stars which eventually form thecentral bulge are not born in superclusters which then sink to the center ofthe galaxy, because feedback efficiently disperses GMCs after they turn severalpercent of their mass into stars. Most of the mass that reaches the nucleusdoes so in the form of gas. The Kennicutt-Schmidt law emerges naturally as aconsequence of feedback balancing gravitational collapse, independent of thesmall-scale star formation microphysics. The same mechanisms that drive thisrelation in isolated galaxies, in particular radiation pressure from IRphotons, extend over seven decades in SFR to regulate star formation in themost extreme starbursts (densities >10^4 M_sun/pc^2). Feedback also drivessuper-winds with large mass loss rates; but a significant fraction of the windmaterial falls back onto the disks at later times, leading to higherpost-starburst SFRs in the presence of stellar feedback. Strong AGN feedback isrequired to explain sharp cutoffs in star formation rate. We compare thepredicted relic structure, mass profile, morphology, and efficiency of disksurvival to simulations which do not explicitly resolve GMCs or feedback.Global galaxy properties are similar, but sub-galactic properties and starformation rates can differ significantly.

Star Formation in Galaxy Mergers with Realistic Models of Stellar Feedback & the Interstellar Medium