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We study the occurrence of delayed SNe~Ia in the single degenerate (SD)scenario. We assume that a massive carbon-oxygen (CO) white dwarf (WD) accretesmatter coming from a companion star, making it to spin at the critical rate. Weassume uniform rotation due to magnetic field coupling. The carbon ignitionmass for non-rotating WDs is M_{ig}^{NR} \approx 1.38 M_{\odot}; while for thecase of uniformly rotating WDs it is a few percent larger (M_{ig}^{R} \approx1.43 M_{\odot}). When accretion rate decreases, the WD begins to lose angularmomentum, shrinks, and spins up; however, it does not overflow its criticalrotation rate, avoiding mass shedding. Thus, angular momentum losses can leadthe CO WD interior to compression and carbon ignition, which would induce anSN~Ia. The delay, largely due to the angular momentum losses timescale, may belarge enough to allow the companion star to evolve to a He WD, becomingundetectable at the moment of explosion. This scenario supports the occurrenceof delayed SNe~Ia if the final CO WD mass is 1.38 M_{\odot} < M < 1.43M_{\odot}. We also find that if the delay is longer than ~3 Gyr, the WD wouldbecome too cold to explode, rather undergoing collapse.

Final Evolution and Delayed Explosions of Spinning White Dwarfs in Single Degenerate Models for Type Ia Supernovae