  We argue that the properties of the Type Ia supernova (SN Ia) SN 2011fe can
be best explained within the frame of the core-degenerate (CD) scenario. In the
CD scenario a white dwarf (WD) merges with the core of an asymptotic giant
branch (AGB) star and forms a rapidly rotating WD, with a mass close to and
above the critical mass for explosion. Rapid rotation prevents immediate
collapse and/or explosion. Spinning down over a time of 0-10 Gyr brings the WD
to explosion. A very long delayed explosion to post-crystallization phase,
which lasts for about 2 Gyr leads to the formation of a highly carbon-enriched
outer layer. This can account for the carbon-rich composition of the
fastest-moving ejecta of SN 2011fe. In reaching the conclusion that the CD
scenario best explains the observed properties of SN 2011fe we consider both
its specific properties, like a very compact exploding object and carbon rich
composition of the fastest-moving ejecta, and the general properties of SNe Ia.
