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Models of poststarburst (or "K+A") galaxies are constructed by combiningfully three-dimensional hydrodynamic simulations of galaxy mergers withradiative transfer calculations of dust attenuation. Spectral line catalogs aregenerated automatically from moderate-resolution optical spectra calculated asa function of merger progress in each of a large suite of simulations. Themass, gas fraction, orbital parameters, and mass ratio of the merging galaxiesare varied systematically, showing that the lifetime and properties of the K+Aphase are strong functions of merger scenario. K+A durations are generally lessthan ~0.1-0.3 Gyr, significantly shorter than the commonly assumed 1 Gyr, whichis obtained only in rare cases, owing to a wide variation in star formationhistories resulting from different orbital and progenitor configurations.Combined with empirical merger rates, the model lifetimes predictrapidly-rising K+A fractions as a function of redshift that are consistent withresults of large spectroscopic surveys, resolving tension between the observedK+A abundance and that predicted when one assumes the K+A duration is thelifetime of A stars (~1 Gyr). The effects of dust attenuation, viewing angle,and aperture bias on our models are analyzed. In some cases, the K+A featuresare longer-lived and more pronounced when AGN feedback removes dust from thecenter, uncovering the young stars formed during the burst. In this picture,the K+A phase begins during or shortly after the bright starburst/AGN phase inviolent mergers, and thus offers a unique opportunity to study the effects ofquasar and star formation feedback on the gas reservoir and evolution of theremnant. Analytic fitting formulae are provided for the estimates of K+Aincidence as a function of merger scenario.

K+A Galaxies as the Aftermath of Gas-Rich Mergers: Simulating the Evolution of Galaxies as Seen by Spectroscopic Surveys