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Low-mass helium-core white-dwarfs (WDs) with masses below 0.5 Msun are knownto be formed in binary star systems but unexpectedly a significant fraction ofthem seem to be single. On the other hand, in Cataclysmic Variables (CVs) alarge number of low-mass WD primary stars is predicted but not observed. Werecently showed that the latter problem can be solved if consequential angularmomentum loss causes especially CVs with low-mass WDs to merge and form singlestars. Here we simulate the population of single WDs resulting from single starevolution and from binary star mergers taking into account these new mergingCVs. We show that according to the revised model of CV evolution, merging CVsmight be the dominant channel leading to the formation of low-mass single WDsand that the predicted relative numbers are consistent with observations. Thiscan be interpreted as further evidence for the revised model of CV evolution werecently suggested. This model includes consequential angular momentum lossthat increases with decreasing WD mass and might not only explain the absenceof low-mass WD primaries in CVs but also the existence of single low-mass WDs.

The origin of single low-mass WDs: another problem that consequential angular momentum loss in CVs might solve