`Tail-end' Bondi-Hoyle accretion in young star clusters: Implications for disks, planets, and stars

TL;DR

This study investigates Bondi-Hoyle accretion onto disks in young star clusters through simulations, revealing significant accretion rates that could influence disk evolution, planet formation, and stellar composition.

Contribution

It presents the first detailed N-body simulations of Bondi-Hoyle accretion in young clusters, quantifying accretion rates onto disks and their potential impact on planetary system development.

Findings

Disks around solar-mass stars accrete ~0.01 M_sun per Myr in small clusters.

Accretion rates scale as M^2.1 with stellar mass.

Higher cluster stellar velocities reduce accretion rates.

Abstract

Young stars orbiting in the gravitational potential well of forming star clusters pass through the cluster's dense molecular gas and can experience Bondi-Hoyle accretion from reservoirs outside their individual protostellar cloud cores. Accretion can occur for several million years after the stars form, but before the cluster disperses. This accretion is predominantly onto the disk and not the star. N-body simulations of stars orbiting in three young model clusters containing 30, 300, and 3000 stars are presented. The simulations include the gravitational potential of the molecular gas which smoothly disperses over time. The clusters have a star formation efficiency of 33% and a radius of 0.22 pc. We find that the disks surrounding solar-mass stars in the N=30 cluster accretes ~0.01 M_sol (~1 minimum-mass solar nebula, MMSN) per Myr. The accretion rate scales as M^2.1 for stars of mass M. The accretion rate is ~5 times lower for N=3000 cluster, due to its higher stellar velocities and higher temperature. The Bondi-Hoyle accretion rates onto the disks are several times lower than accretion rates observed directly onto young stars (e.g., Muzerolle et al 2005): these two accretion rates follow the same M^2 behavior and may be related. The accreted disk mass is large enough that it may have a substantial and unappreciated effect on disk structure and the formation of planetary systems. We discuss a variety of implications of this process, including its effect on metallicity differences between cluster stars, compositional differences between a star and its disk, the formation of terrestrial and gas-giant planets, and isotopic anomalies observed in our Solar System.