  Even though Type Ia supernovae (SNIa) play an important role in many fields
in astronomy, the nature of the progenitors of SNIa remain a mystery. One of
the classical evolutionary pathways towards a SNIa explosion is the single
degenerate (SD) channel, in which a carbon-oxygen white dwarf accretes matter
from its non-degenerate companion until it reaches the Chandrasekhar mass.
Constraints on the contribution from the SD channel to the overall SNIa rate
come from a variety of methods, e.g. from abundances, from signatures of the
companion star in the light curve or near the SNIa remnant, and from synthetic
SNIa rates. In this proceedings, I show that when incorporating our newest
understandings of binary evolution, the SNIa rate from the single degenerate
channel is enhanced. I also discuss the applicability of these constraints on
the evolution of SNIa progenitors.
