We investigate if consequential angular momentum losses ( CAML ) or an intrinsic deformation of the donor star in CVs could increase the CV bounce period from the canonical theoretical value \sim 65 min to the observed value P _ { min } \approx 77 min , and if a variation of these effects in a CV population could wash out the theoretically predicted accumulation of systems near the minimum period ( the period spike ) .
We are able to construct suitably mixed CV model populations that a statisticial test can not rule out as the parent population of the observed CV sample .
However , the goodness of fit is never convincing , and always slightly worse than for a simple , flat period distribution .
Generally , the goodness of fit is much improved if all CVs are assumed to form at long orbital periods .
The weighting suggested by King , Schenker & Hameury ( 2002 ) does not constitute an improvment if a realistically shaped input period distribution is used .