REGULATION OF STAR FORMATION RATES IN MULTIPHASE GALACTIC DISKS: NUMERICAL TESTS OF THE THERMAL/DYNAMICAL EQUILIBRIUM MODEL

We use vertically resolved numerical hydrodynamic simulations to study star formation and the interstellar medium (ISM) in galactic disks. We focus on outer-disk regions where diffuse HI dominates, with gas surface densities Sigma = 3-20 M-circle dot pc(-2) and star-plus-dark matter volume densities rho(sd) = 0.003-0.5 M-circle dot pc(-3). Star formation occurs in very dense, self-gravitating clouds that form by mergers of smaller cold cloudlets. Turbulence, driven by momentum feedback from supernova events, destroys bound clouds and puffs up the disk vertically. Time-dependent radiative heating (FUV from recent star formation) offsets gas cooling. We use our simulations to test a new theory for self-regulated star formation. Consistent with this theory, the disks evolve to a state of vertical dynamical equilibrium and thermal equilibrium with bothwarm and cold phases. The range of star formation surface densities and midplane thermal pressures is Sigma(SFR) similar to 10(-4) to 10(-2) M-circle dot kpc(-2) yr(-1) and P-th/k(B) similar to 10(2) to 10(4) cm(-3) K. In agreement with observations, turbulent velocity dispersions are similar to 7 km s(-1) and the ratio of the total (effective) to thermal pressure is P-tot/P-th similar to 4-5, across this whole range (provided shielding is similar to the solar neighborhood). We show that Sigma(SFR) is not well correlated with Sigma alone, but rather with Sigma root rho(sd), because the vertical gravity from stars and dark matter dominates in outer disks. We also find that Sigma(SFR) has a strong, nearly linear correlation with P-tot, which itself is within similar to 13% of the dynamical equilibrium estimate P-tot,P-DE. The quantitative relationships we find between Sigma(SFR) and the turbulent and thermal pressures show that star formation is highly efficient for energy and momentum production, in contrast to the low efficiency of mass consumption. Star formation rates adjust until the ISM's energy and momentum losses are replenished by feedback within a dynamical time.