Bondi-Hoyle-Lyttleton Accretion onto a Protoplanetary Disk

TL;DR

This study uses hydrodynamic simulations to explore how dense interstellar medium accretion affects protoplanetary disks around young stars, revealing structural changes and potential impacts on planet formation.

Contribution

It provides the first detailed hydrodynamic analysis of accretion onto star-disk systems, highlighting effects on disk structure and dynamics not captured by classical models.

Findings

Outer disk migrates inward, increasing inner disk density

Spiral density features develop in the disk

Accretion rate onto the star remains roughly constant

Abstract

Young stellar systems orbiting in the potential of their birth cluster can accrete from the dense molecular interstellar medium during the period between the star's birth and the dispersal of the cluster's gas. Over this time, which may span several Myr, the amount of material accreted can rival the amount in the initial protoplanetary disk; the potential importance of this `tail-end' accretion for planet formation was recently highlighted by Throop & Bally (2008). While accretion onto a point mass is successfully modeled by the classical Bondi-Hoyle-Lyttleton solutions, the more complicated case of accretion onto a star-disk system defies analytic solution. In this paper we investigate via direct hydrodynamic simulations the accretion of dense interstellar material onto a star with an associated gaseous protoplanetary disk. We discuss the changes to the structure of the accretion flow caused by the disk, and vice versa. We find that immersion in a dense accretion flow can redistribute disk material such that outer disk migrates inwards, increasing the inner disk surface density and reducing the outer radius. The accretion flow also triggers the development of spiral density features, and changes to the disk inclination. The mean accretion rate onto the star remains roughly the same with and without the presence of a disk. We discuss the potential impact of this process on planet formation, including the possibility of triggered gravitational instability; inclination differences between the disk and the star; and the appearance of spiral structure in a gravitationally stable system.