Debris disk size distributions: steady state collisional evolution with P-R drag and other loss processes

TL;DR

This paper introduces a fast, steady-state model for the size distribution of debris disks considering collisional cascades and loss processes like P-R drag, improving understanding of disk evolution and observability.

Contribution

The authors develop a new, efficient scheme for modeling steady-state size distributions in debris disks, incorporating various loss processes and validated against expected theoretical behaviors.

Findings

Reproduces two-phase size distribution with ripples above blow-out size

Predicts disk and dust mass evolution over time

Shows P-R drag causes a size distribution turnover at small sizes

Abstract

We present a new scheme for determining the shape of the size distribution, and its evolution, for collisional cascades of planetesimals undergoing destructive collisions and loss processes like Poynting-Robertson drag. The scheme treats the steady state portion of the cascade by equating mass loss and gain in each size bin; the smallest particles are expected to reach steady state on their collision timescale, while larger particles retain their primordial distribution. For collision-dominated disks, steady state means that mass loss rates in logarithmic size bins are independent of size. This prescription reproduces the expected two phase size distribution, with ripples above the blow-out size, and above the transition to gravity-dominated planetesimal strength. The scheme also reproduces the expected evolution of disk mass, and of dust mass, but is computationally much faster than evolving distributions forward in time. For low-mass disks, P-R drag causes a turnover at small sizes to a size distribution that is set by the redistribution function (the mass distribution of fragments produced in collisions). Thus information about the redistribution function may be recovered by measuring the size distribution of particles undergoing loss by P-R drag, such as that traced by particles accreted onto Earth. Although cross-sectional area drops with 1/age^2 in the PR-dominated regime, dust mass falls as 1/age^2.8, underlining the importance of understanding which particle sizes contribute to an observation when considering how disk detectability evolves. Other loss processes are readily incorporated; we also discuss generalised power law loss rates, dynamical depletion, realistic radiation forces and stellar wind drag.