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We examine the effect of mass and force resolution on a specific starformation (SF) recipe using a set of N-body/Smooth Particle Hydrodynamicsimulations of isolated galaxies. Our simulations span halo masses from 10^9 to10^13 solar masses, more than four orders of magnitude in mass resolution, andtwo orders of magnitude in the gravitational softening length, epsilon,representing the force resolution. We examine the total global star formationrate, the star formation history, and the quantity of stellar feedback andcompare the disk structure of the galaxies. Based on our analysis, we recommendusing at least 10^4 particles each for the dark matter and gas component and aforce resolution of epsilon approximately equal to 10^-3 R_vir when studyingglobal SF and feedback. When the spatial distribution of stars is important,the number of gas and dark matter particles must be increased to at least 10^5of each. Low mass resolution simulations with fixed softening lengths showparticularly weak stellar disks due to two-body heating. While decreasingspatial resolution in low mass resolution simulations limits two-body effects,density and potential gradients cannot be sustained. Regardless of thesoftening, low-mass resolution simulations contain fewer high density regionswhere SF may occur. Galaxies of approximately 10^10 solar masses display uniquesensitivity to both mass and force resolution. This mass of galaxy has ashallow potential and is on the verge of forming a disk. The combination ofthese factors give this galaxy the potential for strong gas outflows driven bysupernova feedback and make it particularly sensitive to any changes to thesimulation parameters.

Star Formation and Feedback in Smoothed Particle Hydrodynamic Simulations II: Resolution Effects