  I study the rate of type Ia supernovae (SNe Ia) within about a million years
after the assumed common envelope evolution (CEE) that forms the progenitors of
these SNe Ia, and find that the population of SNe Ia with short CEE to
explosion delay (CEED) time is ~fewx0.1 of all SNe Ia. I also claim for an
expression for the rate of these SNe Ia that occur at short times after the
CEE, t(CEED)<10^6 year, that is different from that of the delay time
distribution (DTD) billions of years after star formation. This tentatively
hints that the physical processes that determine the short CEED time
distribution (CEEDTD) are different (at least to some extend) from those that
determine the DTD at billions of years. To reach these conclusions I examine
SNe Ia that interact with a circumstellar matter (CSM) within months after
explosion, so called SNe Ia-CSM, and the rate of SNe Ia that on a time scale of
tens to hundreds of years interact with a CSM that might have been a planetary
nebula, so called SNe Ia inside a planetary nebula (SNIPs). I assume that the
CSM in these populations results from a CEE, and hence this study is relevant
mainly to the core degenerate (CD) scenario, to the double degenerate (DD)
scenario, to the double detonation (DDet) scenario with white dwarf companions,
and to the CEE-wind channel of the single degenerate (SD) scenario.
