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We investigate here populations of cataclysmic variables (CVs) in a set of288 globular cluster (GC) models evolved with the MOCCA code. This is by farthe largest sample of GC models ever analysed with respect to CVs. Contrary towhat has been argued for a long time, we found that dynamical destruction ofprimordial CV progenitors is much stronger in GCs than dynamical formation ofCVs, and that dynamically formed CVs and CVs formed under no/weak influence ofdynamics have similar white dwarf mass distributions. In addition, we foundthat, on average, the detectable CV population is predominantly composed of CVsformed via typical common envelope phase (CEP) ($\gtrsim70$ per cent), thatonly $\approx2-4$ per cent of all CVs in a GC is likely to be detectable, andthat core-collapsed models tend to have higher fractions of bright CVs thannon-core-collapsed ones. We also consistently show, for the first time, thatthe properties of bright and faint CVs can be understood by means of the pre-CVand CV formation rates, their properties at their formation times and clusterhalf-mass relaxation times. Finally, we show that models following the initialbinary population proposed by Kroupa and set with low CEP efficiency betterreproduce the observed amount of CVs and CV candidates in NGC 6397, NGC 6752and 47 Tuc. To progress with comparisons, the essential next step is toproperly characterize the candidates as CVs (e.g. by obtaining orbital periodsand mass ratios).

monthly notices of the royal astronomical society

MOCCA-SURVEY database I. Accreting white dwarf binary systems in  globular clusters -- IV. cataclysmic variables -- properties of bright and  faint populations