Comparison of theoretical white dwarf cooling timescales

TL;DR

This study compares white dwarf cooling times from two independent stellar evolution codes, achieving a 2% accuracy level, which helps refine white dwarf cosmochronology and supports future observational and theoretical research.

Contribution

First direct comparison of two widely used white dwarf evolution codes with identical physics, establishing a maximum accuracy benchmark for cooling time estimates.

Findings

Achieved 2% agreement in cooling times at low luminosities

Confirmed robustness of results across different core compositions

Provided tabulated cooling sequences for future code validation

Abstract

An accurate assessment of white dwarf cooling times is paramount to place white dwarf cosmochronology of Galactic populations on more solid grounds. This issue is particularly relevant in view of the enhanced observational capabilities provided by the next generation of Extremely Large Telescopes, that will offer more avenues to employ white dwarfs as probes of Galactic evolution and test-beds of fundamental physics. We estimate for the first time the consistency of results obtained from two independent and widely used evolutionary codes (BaSTI and LPCODE) for white dwarf models with fixed mass and chemical stratification, when the same input physics is employed in both codes. We considered 0.55Msun white dwarf models with both pure carbon and uniform carbon-oxygen (50/50 mass fractions) core. We have assessed for the first time the maximum possible accuracy in the current estimates of white dwarf cooling times, resulting only from the different implementations of the stellar evolution equations and homogeneous input physics in two independent stellar evolution codes. This accuracy amounts to 2% at luminosities lower than log(L/L_{\sun})= -1.5$. This agreement is true for both pure carbon and uniform carbon-oxygen stratification core models, and also when the release of latent heat and carbon-oxygen phase separation are considered. This difference is smaller than the uncertainties in cooling times due to the present uncertainties in the white dwarf chemical stratification. We have also determined quantitatively and explained the effect of varying equation of state, low-temperature radiative opacities and electron conduction opacities in our calculation. Finally, we extend the scope of our work by providing tabulations of our cooling sequences and the required input physics, that can be used as a comparison test of cooling times obtained from other white dwarf evolutionary codes.