A comprehensive population synthesis study of post-common envelope binaries

TL;DR

This study uses population synthesis models to analyze post-common envelope binaries, comparing different theoretical approaches and energy considerations to match observed populations and orbital period distributions.

Contribution

It evaluates the effectiveness of energy and angular momentum budget models in reproducing observed PCEB populations, highlighting the strengths of the energy budget approach with specific initial mass ratio distributions.

Findings

Constant $\alpha_{CE}$ can explain late-type secondaries.

Thermal and ionization energy inclusion improves IK Pegasi modeling.

Canonical energy budget with certain initial mass ratios aligns well with observations.

Abstract

We apply population synthesis techniques to calculate the present day population of post-common envelope binaries (PCEBs) for a range of theoretical models describing the common envelope (CE) phase. Adopting the canonical energy budget approach we consider models where the ejection efficiency, $\alpha_{\rmn{CE}}$ is either a constant, or a function of the secondary mass. We obtain the envelope binding energy from detailed stellar models of the progenitor primary, with and without the thermal and ionization energy, but we also test a commonly used analytical scaling. We also employ the alternative angular momentum budget approach, known as the $\gamma$-algorithm. We find that a constant, global value of $\alpha_{\rmn{CE}} \ga 0.1$ can adequately account for the observed population of PCEBs with late spectral-type secondaries. However, this prescription fails to reproduce IK Pegasi, which has a secondary with spectral type A8. We can account for IK Pegasi if we include thermal and ionization energy of the giant's envelope, or if we use the $\gamma$-algorithm. However, the $\gamma$-algorithm predicts local space densities that are 1 to 2 orders of magnitude greater than estimates from observations. In contrast, the canonical energy budget prescription with an initial mass ratio distribution that favours unequal initial mass ratios gives a local space density which is in good agreement with observations, and best reproduces the observed distribution of PCEBs. Finally, all models fail to reproduce the sharp decline for orbital periods, $P_{\rmn{orb}} \ga 1$ d in the orbital period distribution of observed PCEBs, even if we take into account selection effects against systems with long orbital periods and early spectral-type secondaries.