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In this first of a series of papers related to long-periodpost-common-envelope (CE) binaries, we investigated whether extra energy isrequired or not to explain the currently known post-CE binaries withsufficiently long orbital periods consisting of oxygen-neon white dwarfs withAFGK-type main-sequence star companions. We carried out binary populationsimulations with the BSE code and searched for their formation pathways. Unlikewhat has been claimed for a long time, we show that all such post-CE binariescan be explained by assuming inefficient CE evolution, which is consistent withresults achieved for the remaining post-CE binaries. There is therefore no needfor an extra energy source. We also found that for CE efficiency close to 100%,post-CE binaries hosting oxygen-neon white dwarfs with orbital periods as longas a thousand days can be explained. For all known systems we found formationpathways consisting of CE evolution triggered when a highly evolved (i.e. theenvelope mass being comparable to the core mass) thermally-pulsing asymptoticgiant branch star fills its Roche lobe at an orbital period of several thousanddays. Due to the sufficiently low envelope mass and sufficiently long orbitalperiod, the resulting post-CE orbital period can easily be several tens ofdays. We conclude that the known post-CE binaries with oxygen-neon white dwarfsand AFGK-type main-sequence stars can be explained without invoking any energysource other than orbital and thermal energy. Our results strengthen the ideathat the most common formation pathway of the overall population of post-CEbinaries hosting white dwarfs is through inefficient CE evolution.

Formation of long-period post-common-envelope binaries I. No extra  energy is needed to explain oxygen-neon white dwarfs paired with AFGK-type  main-sequence stars