An Unstable Truth: How Massive Stars get their Mass

TL;DR

This paper introduces a new high-accuracy radiation simulation method to study massive star formation, revealing that gravitational and Rayleigh-Taylor instabilities play a crucial role in mass accretion, especially in turbulent environments.

Contribution

The authors develop a novel radiation algorithm that accurately models direct stellar radiation and dust re-emission, enabling detailed 3D simulations of massive star formation with resolved instabilities.

Findings

Mass is channeled via gravitational and RT instabilities.

Proper radiation treatment delays but does not prevent instabilities.

Turbulence seeds immediate instabilities during collapse.

Abstract

The pressure exerted by massive stars' radiation fields is an important mechanism regulating their formation. Detailed simulation of massive star formation therefore requires an accurate treatment of radiation. However, all published simulations have either used a diffusion approximation of limited validity; have only been able to simulate a single star fixed in space, thereby suppressing potentially-important instabilities; or did not provide adequate resolution at locations where instabilities may develop. To remedy this we have developed a new, highly accurate radiation algorithm that properly treats the absorption of the direct radiation field from stars and the re-emission and processing by interstellar dust. We use our new tool to perform three-dimensional radiation-hydrodynamic simulations of the collapse of massive pre-stellar cores with laminar and turbulent initial conditions and properly resolve regions where we expect instabilities to grow. We find that mass is channeled to the stellar system via gravitational and Rayleigh-Taylor (RT) instabilities, in agreement with previous results using stars capable of moving, but in disagreement with methods where the star is held fixed or with simulations that do not adequately resolve the development of RT instabilities. For laminar initial conditions, proper treatment of the direct radiation field produces later onset of instability, but does not suppress it entirely provided the edges of radiation-dominated bubbles are adequately resolved. Instabilities arise immediately for turbulent pre-stellar cores because the initial turbulence seeds the instabilities. Our results suggest that RT features are significant and should be present around accreting massive stars throughout their formation.