# Radiation hydrodynamic simulations of massive star formation via gravitationally trapped HII regions - Spherically symmetric ionised accretion flows

## TL;DR

This study uses radiation hydrodynamical simulations to explore how gravitationally trapped HII regions evolve during massive star formation, revealing instabilities and a transition from accretion to expansion phases.

## Contribution

It provides the first detailed simulations of spherically symmetric ionised accretion flows including gravity, demonstrating the evolution from trapped to expanding HII regions in massive star formation.

## Key findings

- Gravitationally trapped HII regions exist with accretion through the ionisation front.
- Ionisation front fluctuations are unstable in spherical symmetry.
- Expansion of HII regions halts accretion and star growth.

## Abstract

This paper investigates the gravitational trapping of HII regions predicted by steady-state analysis using radiation hydrodynamical simulations. We present idealised spherically symmetric radiation hydrodynamical simulations of the early evolution of HII regions including the gravity of the central source. As with analytic steady state solutions of spherically symmetric ionised Bondi accretion flows, we find gravitationally trapped HII regions with accretion through the ionisation front onto the source. We found that, for a constant ionising luminosity, fluctuations in the ionisation front are unstable. This instability only occurs in this spherically symmetric accretion geometry. In the context of massive star formation, the ionising luminosity increases with time as the source accretes mass. The maximum radius of the recurring HII region increases on the accretion timescale until it reaches the sonic radius, where the infall velocity equals the sound speed of the ionised gas, after which it enters a pressure-driven expansion phase. This expansion prevents accretion of gas through the ionisation front, the accretion rate onto the star decreases to zero, and it stops growing from accretion. Because of the time required for any significant change in stellar mass and luminosity through accretion our simulations keep both mass and luminosity constant and follow the evolution from trapped to expanding in a piecewise manner. Implications of this evolution of HII regions include a continuation of accretion of material onto forming stars for a period after the star starts to emit ionising radiation, and an extension of the lifetime of ultracompact HII regions.