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We present a theoretical delay time distribution (DTD) of Type Ia supernovaeon the basis of our new evolutionary models of single degenerate (SD)progenitor systems. Our model DTD has almost a featureless power law shape(\propto t^{-n} with n \approx 1) for the delay time from t \sim 0.1 to 10 Gyr.This is in good agreement with the recent direct measurement of DTD. Theobserved featureless property of the DTD has been suggested to be favorable forthe double degenerate (DD) scenario but not for the SD scenario. If the massrange of the companion star to the white dwarf (WD) were too narrow in the SDmodel, its DTD would be too limited around the companion's main-sequencelifetime to be consistent with the observed DTD. However, this is not the casein our SD model that consists of the two channels of WD + RG (red giant) and WD+ MS (main-sequence star). In these channels, the companion stars have a massrange of \sim 0.9-3 M_\sun (WD+RG) and \sim 2- 6 M_\sun (WD+MS). The combinedmass range is wide enough to yield the featureless DTD. We emphasize that theSD scenario should include two important processes: the optically thick windsfrom the mass-accreting WD and the mass-stripping from the companion star bythe WD wind.

The Delay Time Distribution of Type Ia Supernovae and the Single Degenerate Model