# Speaking with one voice: simulations and observations discuss the common envelope $\alpha$ parameter

## TL;DR

This study compares hydrodynamic simulations of the common envelope phase with observations of post-common envelope binaries to evaluate the predictive power of the $\alpha$ parameter, revealing limitations and potential correlations.

## Contribution

It provides a comprehensive comparison between simulations and observations, assessing the $\alpha$ parameter's applicability and identifying gaps in current modeling of common envelope interactions.

## Key findings

- Simulations suggest $\alpha_{CE} < 0.6-1.0$, with some indicating $\alpha_{CE} < 0.2$.
- Post-RGB observations align with certain simulations, while post-AGB observations imply lower $\alpha_{CE}$ values.
- Surviving companions have masses above 0.05-0.1 solar masses.

## Abstract

We present a comparative study between the results of most hydrodynamic simulations of the common envelope binary interaction to date and observations of post common envelope binaries. The goal is to evaluate whether this dataset indicates the existence of a formula that may predict final separations of post-common envelope systems as a function of pre-common envelope parameters. Some of our conclusions are not surprising while others are more subtle. We find that: (i) Values of the final orbital separation derived from common envelope simulations must at this time be considered upper limits. Simulations that include recombination energy do not seem to have systematically different final separations; these and other simulations imply $\alpha_{\rm CE} < 0.6-1.0$. At least one simulation, {applicable to double-degenerate systems}, implies $\alpha_{\rm CE} < 0.2$. (ii) Despite large reconstruction errors, the post-RGB observations reconstructed parameters are in agreement with some of the simulations. The post-AGB observations behave instead as if they had a systematically lower value of $\alpha_{\rm CE}$. The lack of common envelope simulations with low mass AGB stars leaves us with no insight as to why this is the case. (iii) The smallest mass companion that survives the common envelope with intermediate mass giants is 0.05-0.1~\ms. (iv) Observations of binaries with separations larger than $\sim$10~\rs, tend to have high $M_2/M_1$ mass ratios and may go through a relatively long phase of unstable Roche lobe mass transfer followed by a weakened common envelope (or with no common envelope at all). (v) The effect of the spatial resolution and of the softening length on simulation results remains poorly quantified.