Abstract
Evidence for current low-level star formation in elliptical galaxies is briefly reviewed. Results of numerical 1-D and 2-D hydrodynamical calculations of the evolution of the interstellar gas in elliptical systems under various assumptions of the dependence of the star formation rate on the local environment are discussed and, when applicable, contrasted with observations. It is possible that elliptical galaxies with very little rotation can produce a single very massive gaseous object (M > 105 M⊙) at the center. A rotating elliptical galaxy, however, invariably produces a disk out of which stars can form. Star formation under these conditions should be intermittent.
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