# Collisions and drag in debris discs with eccentric parent belts

## TL;DR

This study investigates how collisions and drag forces influence asymmetries in debris discs with eccentric belts, revealing complex interactions that affect observable features and spectral energy distributions over long timescales.

## Contribution

It extends a numerical model to include azimuthal variations, analyzing the combined effects of eccentricity, collisions, and drag on debris disc morphology and observables.

## Key findings

- Radiation pressure causes size-dependent asymmetries in the halo.
- Collisional equilibrium favors smaller grains on the apastron side.
- Poynting-Robertson drag creates a more tenuous interior region on the apastron side.

## Abstract

Context: High-resolution images of circumstellar debris discs reveal off-centred rings that indicate past or ongoing perturbation, possibly caused by secular gravitational interaction with unseen stellar or substellar companions. The purely dynamical aspects of this departure from radial symmetry are well understood. However, the observed dust is subject to additional forces and effects, most notably collisions and drag. Aims: To complement the studies of dynamics, we therefore aim to understand how new asymmetries are created by the addition of collisional evolution and drag forces, and existing ones strengthened or overridden. Methods: We augmented our existing numerical code "Analysis of Collisional Evolution" (ACE) by an azimuthal dimension, the longitude of periapse. A set of fiducial discs with global eccentricities ranging from 0 to 0.4 is evolved over giga-year timescales. Size distribution and spatial variation of dust are analysed and interpreted. The basic impact of belt eccentricity on spectral energy distributions (SEDs) and images is discussed. Results: We find features imposed on characteristic timescales. First, radiation pressure defines size cutoffs that differ between periapse and apoapse, resulting in an asymmetric halo. The differences in size distribution make the observable asymmetry of the halo depend on wavelength. Second, collisional equilibrium prefers smaller grains on the apastron side of the parent belt, reducing the effect of pericentre glow and the overall asymmetry. Third, Poynting-Robertson drag fills the region interior to an eccentric belt such that the apastron side is more tenuous. Interpretation and prediction of the appearance in scattered light is problematic when spatial and size distribution are coupled.