Dependence of a planet's chaotic zone on particle eccentricity: the shape of debris disc inner edges

TL;DR

This paper extends the understanding of a planet's chaotic zone by incorporating particle eccentricity, showing that higher eccentricities enlarge the zone and affect planetary mass estimates from debris disc edges.

Contribution

The study introduces a modified analytical model for the chaotic zone width that accounts for particle eccentricity, validated by numerical simulations and applied to the HR8799 system.

Findings

Chaotic zone width increases with particle eccentricity above a critical value.

Classical model works for low-eccentricity particles but underestimates zone size at higher eccentricities.

Planet mass estimates from debris disc truncation are significantly affected by particle eccentricity.

Abstract

The orbit of a planet is surrounded by a chaotic zone wherein nearby particles' orbits are chaotic and unstable. Wisdom (1980) showed that the chaos is driven by the overlap of mean motion resonances which occurs within a distance (da/a)_chaos = 1.3 mu^2/7 of the planet's orbit. However, the width of mean motion resonances grows with the particles' eccentricity, which will increase the width of the chaotic zone at higher eccentricities. Here we investigate the width of the chaotic zone using the iterated encounter map and N-body integrations. We find that the classical prescription works well for particles on low-eccentricity orbits. However, above a critical eccentricity, dependent upon the mass of the planet, the width of the chaotic zone increases with eccentricity. An extension of Wisdom's analytical arguments then shows that, above the critical eccentricity, the chaotic zone width is given by (da/a)_chaos = 1.8 e^1/5 mu^1/5, which agrees well with the encounter map results. The critical eccentricity is given by e_cr = 0.21 mu^3/7. This extended chaotic zone results in a larger cleared region when a planet sculpts the inner edge of a debris disc comprised of eccentric planetesimals. Hence, the planet mass estimated from the classical chaotic zone may be erroneous. We apply this result to the HR8799 system, showing that the masses of HR8799b inferred from the truncation of the disc may vary by up to 50% depending on the disc particles' eccentricities. With a disc edge at 90AU, the necessary mass of planet b to cause the truncation would be 8-10 Jovian masses if the disc particles have low eccentricities (<0.02), but only 4-8 Jovian masses if the disc particles have higher eccentricities. Our result also has implications for the ability of a planet to feed material into an inner system, a process which may explain metal pollution in White Dwarf atmospheres.