Stripping a debris disk by close stellar encounters in an open stellar cluster

TL;DR

This study investigates how close stellar encounters in dense open clusters can strip debris disks of planetesimals, significantly affecting their dust production and detectability over 100 million years.

Contribution

It quantifies the impact of stellar flybys on debris disk planetesimals in various cluster environments, highlighting the importance of initial star density.

Findings

Disks in low-density clusters suffer minimal planetesimal loss.

High-density clusters cause severe depletion of debris disks, especially around M-dwarfs.

Approximately two-thirds of stars form in high-density clusters affecting debris disk evolution.

Abstract

A debris disk is a constituent of any planetary system surrounding a main sequence star. We study whether close stellar encounters can disrupt and strip a debris disk of its planetesimals in the expanding open cluster of its birth with a decreasing star number density over 100 Myrs. Such stripping would affect the dust production and hence detectability of the disk. We tabulated the fractions of planetesimals stripped off during stellar flybys of miss distances between 100 and 1000 AU and for several mass ratios of the central to passing stars. We then estimated the numbers of close stellar encounters over the lifetime of several expanding open clusters characterized by their initial star densities. We found that a standard disk, with inner and outer radii of 40 and 100 AU, suffers no loss of planetesimals over 100 Myrs around a star born in a common embedded cluster with star density <1000 pc^-3. In contrast, we found that such a disk is severely depleted of its planetesimals over this timescale around a star born in an Orion-type cluster where the star density is >20 000 pc^-3. In this environment, a disk loses >97% of its planetesimals around an M-dwarf, >63% around a solar-type star, and >42% around an A-dwarf, over 100 Myrs. We roughly estimate that two-thirds of the stars may be born in such high star density clusters. This might explain in part why fewer debris disks are observed around lower mass stars.