White dwarf pollution by planets in stellar binaries

TL;DR

This paper proposes that Lidov-Kozai oscillations induced by binary companions, amplified by stellar mass loss, can explain long-term white dwarf pollution by planetary material, aligning with observed accretion rates and pollution fractions.

Contribution

It introduces a new scenario involving binary-induced Lidov-Kozai oscillations to explain white dwarf pollution at long cooling times, which previous models could not account for.

Findings

Accretion rates match observations for planetary masses between 0.01 and 1 Mars.

Polluted white dwarf fraction in simulations is about 5%, consistent with observations.

Scenario does not explain high pollution fractions at very short or very long cooling times.

Abstract

Approximately $0.2 \pm 0.2$ of white dwarfs (WDs) show signs of pollution by metals, which is likely due to the accretion of tidally disrupted planetary material. Models invoking planet-planet interactions after WD formation generally cannot explain pollution at cooling times of several Gyr. We consider a scenario in which a planet is perturbed by Lidov-Kozai oscillations induced by a binary companion and exacerbated by stellar mass loss, explaining pollution at long cooling times. Our computed accretion rates are consistent with observations assuming planetary masses between $\sim 0.01$ and $1\,M_\mathrm{Mars}$, although nongravitational effects may already be important for masses $\lesssim 0.3 \, M_\mathrm{Mars}$. The fraction of polluted WDs in our simulations, $\sim 0.05$, is consistent with observations of WDs with intermediate cooling times between $\sim 0.1$ and 1 Gyr. For cooling times $\lesssim 0.1$ Gyr and $\gtrsim 1$ Gyr, our scenario cannot explain the high observed pollution fractions of up to 0.7. Nevertheless, our results motivate searches for companions around polluted WDs.