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
arxiv(2024)
摘要
In this first in a series of papers related to long-period
post-common-envelope (CE) binaries, we investigated whether extra energy is
required or not to explain the currently known post-CE binaries with
sufficiently long orbital periods consisting of oxygen-neon white dwarfs with
AFGK-type main-sequence star companions. We carried out binary population
simulations with the BSE code and searched for their formation pathways. Unlike
what has been claimed for a long time, we show that all such post-CE binaries
can be explained by assuming inefficient CE evolution, which is consistent with
results achieved for the remaining post-CE binaries. There is therefore no need
for 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 long
as a thousand days can be explained. For all known systems we found formation
pathways consisting of CE evolution triggered when a highly evolved (i.e. the
envelope mass being comparable to the core mass) thermally-pulsing asymptotic
giant branch star fills its Roche lobe at an orbital period of several thousand
days. Due to the sufficiently low envelope mass and sufficiently long orbital
period, the resulting post-CE orbital period can easily be several tens of
days. We conclude that the known post-CE binaries with oxygen-neon white dwarfs
and AFGK-type main-sequence stars can be explained without invoking any energy
source other than orbital and thermal energy. Our results strengthen the idea
that the most common formation pathway of the overall population of post-CE
binaries hosting white dwarfs is through inefficient CE evolution.
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