  Virtually all close compact binary stars are formed through common-envelope
(CE) evolution. It is generally accepted that during this crucial evolutionary
phase a fraction of the orbital energy is used to expel the envelope. However,
it is unclear whether additional sources of energy, such as the recombination
energy of the envelope, play an important role. Here we report the discovery of
the second and third longest orbital period post-common envelope binaries
(PCEBs) containing white dwarf (WD) primaries, i.e. SDSSJ121130.94-024954.4
(Porb = 7.818 +- 0.002 days) and SDSSJ222108.45+002927.7 (Porb = 9.588 +- 0.002
days), reconstruct their evolutionary history, and discuss the implications for
the energy budget of CE evolution. We find that, despite their long orbital
periods, the evolution of both systems can still be understood without
incorporating recombination energy, although at least small contributions of
this additional energy seem to be likely. If recombination energy significantly
contributes to the ejection of the envelope, more PCEBs with relatively long
orbital periods (Porb >~ 1-3 day) harboring massive WDs (Mwd >~ 0.8 Msun)
should exist.
