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Star formation and chemical enrichment histories of the dwarf spheroidalgalaxies (dSphs) Draco, Sextans, and Ursa Minor are investigated by means ofchemical evolution models and a simulation code for colour-magnitude diagrams(CMDs). The CMD simulation code is designed to fully consider effects of thechemical evolution on stellar evolution and photometric properties. Comparisonsbetween the chemical evolution models and the observed abundance patternsreveal that the star formation rates were very low (1-5% of that of the solarneighbourhood disc) and that the initial star formation continued for a longduration (> 3.9-6.5 Gyr) in these dSphs. This star formation history canreproduce morphologies of the observed CMDs, such as narrow red giant branchesand red horizontal branches. Hence, both of the abundance patterns and themorphologies of the CMDs can be explained by the star formation historiescharacterised by the low star formation rate and the long duration of the starformation period. Because of the low star formation rates, plenty of gasremains at the final epoch of star formation. We suggest that gas stripping bythe Galaxy results in termination of star formation in the dSphs.Comment: 26 pages, Accepted by A&

Extended star formation in dwarf spheroidal galaxies: The cases of Draco, Sextans, and Ursa Minor