How many cataclysmic variables are crossing the period gap?: A test for the disruption of magnetic braking

We apply population synthesis techniques to calculate the present-day number of two types of white-dwarf main-sequence star (WDMS) binaries within the cataclysmic variable 2 to 3 h period gap. The first are post-common envelope binaries with secondary stars that have masses 0.17 <= M(2)/M(circle dot) <= 0.36 gap-post common envelope binaries (gPCEBs), such that they will commence mass transfer within the period gap. The second type are systems that were cataclysmic variables (CVs) at some point in their past, but detached once they evolved down in orbital period to approximate to 3 h as a consequence of disrupted magnetic braking, and are crossing the period gap via gravitational radiation detached cataclysmic variables (dCVs). Full population synthesis calculations are performed where we either assume constant, global values of the common envelope ejection efficiency, alpha CE, or consider alpha CE as a function of secondary mass. Several forms of magnetic braking are also considered. We predict an excess of dCVs over gPCEBs within the period gap of similar to 4 to similar to 13 assuming alpha(CE) = 0.1-0.6, and an initial mass ratio distribution of the form n(q) = 1. This excess is revealed as a prominent peak at the location of the period gap in the orbital period distribution of the combined gPCEB and dCV population. We suggest that if such a feature is observed in the orbital period distribution of an observed sample of short orbital periodWDMS binaries, this would strongly corroborate the disruption of magnetic braking.