  Supernova 2002ic was an atypical Type Ia supernova (SN Ia) with evidence for
substantial amounts of hydrogen associated with the system. Contrary to
previous claims, we show that its unusual properties can be understood within
the framework of one of the most favoured progenitor models, the so-called
supersoft channel. This requires that the donor star was initially relatively
massive ($\sim 3\Ms$) and that the system experienced a delayed dynamical
instability, leading to a large amount of mass loss from the system in the last
few $10^4 $yr before the explosion. This can produce the inferred hydrogen-rich
circumstellar environment, most likely with a disc-like geometry. However, to
apply these models requires a larger accretion efficiency onto the white dwarf
than is assumed in present parameterizations. If this is confirmed, it would
most likely increase estimates for the frequency of the single-degenerate
channel. Based on population synthesis simulations we estimate that not more
than 1 in 100 SNe Ia should belong to this subgroup of SNe Ia.
