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The evolution of an accreting white dwarf (WD) with strong magnetic fieldtoward a type Ia supernova (SN Ia) may differ from the classicalsingle-degenerate (SD) channel. In this paper, we perform binary populationsynthesis (BPS) simulations for the SD channel with a main-sequence (MS)companion, including the strongly magnetized WD accretion. Under a reasonableassumption that the fraction of such systems is $\sim 15$%, the resulting delaytime distribution (DTD) roughly follows the $t^{-1}$ power-law distribution.Within the (WD/MS) SD channel, the contribution from the highly magnetized WDis estimated to be comparable to that from the classical, non-magnetized WDchannel. The contribution of the SD channel toward SNe Ia can be at least $\sim30$% among the whole SN Ia population. We suggest that the SNe Ia resultingfrom the highly-magnetized WD systems would not share observational propertiesexpected for the classical SD channel; for every (potentially peculiar) SNobservationally associated with the SD channel, we expect a comparable numberof the `hidden' SD population in the normal class.

Possible Contribution of Magnetized White Dwarf Binaries to Type Ia Supernova Populations