# Hydrodynamical models of cometary HII regions

## TL;DR

This study models the evolution of cometary HII regions driven by massive stars, exploring how stellar mass and core density influence features like limb-brightening and cavity growth.

## Contribution

It introduces hydrodynamical models of cometary HII regions with off-centre stars in power-law density cores, highlighting the effects of stellar mass on observable features.

## Key findings

- Stars with mass ≥12 M_sun produce limb-brightening.
- Cavity sizes grow and plateau as HII regions evolve.
- Spectral energy distributions are similar to uniform density models.

## Abstract

We have modelled the evolution of cometary HII regions produced by zero-age main-sequence stars of O and B spectral types, which are driving strong winds and are born off-centre from spherically symmetric cores with power-law ($\alpha = 2$) density slopes. A model parameter grid was produced that spans stellar mass, age and core density. Exploring this parameter space we investigated limb-brightening, a feature commonly seen in cometary HII regions. We found that stars with mass $M_\star \geq 12\, \mathrm{M}_\odot$ produce this feature. Our models have a cavity bounded by a contact discontinuity separating hot shocked wind and ionised ambient gas that is similar in size to the surrounding HII region. Due to early pressure confinement we did not see shocks outside of the contact discontinuity for stars with $M_\star \leq 40\, \mathrm{M}_\odot$, but the cavities were found to continue to grow. The cavity size in each model plateaus as the HII region stagnates. The spectral energy distributions of our models are similar to those from identical stars evolving in uniform density fields. The turn-over frequency is slightly lower in our power-law models due to a higher proportion of low density gas covered by the HII regions.