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Recent observations of Type Ia supernovae (SNe Ia) suggest that some of theprogenitor white dwarfs (WDs) had masses up to 2.4-2.8 M_sun, highly exceedingthe Chandrasekhar mass limit. We present a new single degenerate (SD) model forSN Ia progenitors, in which the WD mass possibly reaches 2.3-2.7 M_sun. Threebinary evolution processes are incorporated; optically thick winds frommass-accreting WDs, mass-stripping from the binary companion star by the WDwinds, and WDs being supported by differential rotation. The WD mass canincrease by accretion up to 2.3 (2.7) M_sun from the initial value of 1.1 (1.2)M_sun, being consistent with high luminosity SNe Ia such as SN 2003fg, SN2006gz, SN 2007if, and SN 2009dc. There are three characteristic mass ranges ofexploding WDs. In an extreme massive case, differentially rotating WDs explodeas an SN Ia soon after the WD mass exceeds 2.4 M_sun because of a secularinstability at T/|W|\sim 0.14. For a mid mass range of M_WD=1.5-2.4 M_sun, ittakes some time (spinning-down time) until carbon is ignited to induce an SN Iaexplosion after the WD mass has reached maximum, because it needs a loss orredistribution of angular momentum. For a lower mass case of rigidly rotatingWDs, M_WD=1.38-1.5 M_sun, the spinning-down time depends on the timescale ofangular momentum loss from the WD. The difference in the spinning-down time mayproduce the "prompt" and "tardy" components. We also suggest the very brightsuper-Chandrasekhar mass SNe Ia are born in a low metallicity environment.

A Single Degenerate Progenitor Model for Type Ia Supernovae Highly Exceeding the Chandrasekhar Mass Limit