Star Formation in Isolated Disk Galaxies. I. Models and Star Formation Characteristics

We model star formation in a wide range of isolated disk galaxies composed of a dark matter halo and a disk of stars and isothermal gas, using a threedimensional smoothed particle hydrodynamics code. Absorbing sink particles are used to directly measure the mass of gravitationally collapsing gas. They reach masses characteristic of stellar clusters. In this paper, we describe our galaxy models and numerical methods, followed by an investigation of the gravitational instability in these galaxies. Gravitational collapse forms star clusters with correlated positions and ages, as observed in the Large Magellanic Cloud. Gravitational instability alone acting in unperturbed galaxies appears sufficient to produce flocculent spiral arms, though not more organized patterns. Unstable galaxies show collapse in thin layers in the galactic plane; associated dust will form thin dust lanes in those galaxies, in agreement with observations. We find an exponential relationship between the global star formation timescale and the minimum value in a galaxy of the Toomre instability parameter for a combination of stars and gas Qsg. Furthermore, collapse occurs only in regions with Qsg < 1.6. Our results suggest that vigorous starbursts occur where Qsg ≪ 1, while slow star formation takes place at higher values of Qsg below 1.6. Massive, or gas-rich, galaxies have low initial Qsg, giving high star formation rate, while low-mass, or gas-poor galaxies have high initial Qsg, giving low star formation rate. Subject headings: galaxy: evolution — galaxy: spiral — galaxy: kinematics and dynamics — galaxy: ISM — galaxy: star clusters — stars: formation