Line Emission from Radiation-Pressurized HII Regions I: Internal Structure and Line Ratios

TL;DR

This paper models the internal structure of HII regions considering radiation pressure and stellar winds, revealing how these factors influence emission line ratios and the ionization parameter saturation.

Contribution

It introduces a grid of quasi-static HII region models that incorporate radiation pressure and stellar winds, clarifying their effects on emission line diagnostics.

Findings

Radiation pressure causes saturation in line ratios at high luminosities.

Strong stellar winds limit the maximum ionization parameter.

Some models assuming wind-blown bubbles are inconsistent with high ionization parameters.

Abstract

The emission line ratios [OIII]5007/H-beta and [NII]6584/H-alpha have been adopted as an empirical way to distinguish between the fundamentally different mechanisms of ionization in emission-line galaxies. However, detailed interpretation of these diagnostics requires calculations of the internal structure of the emitting HII regions, and these calculations depend on the assumptions one makes about the relative importance of radiation pressure and stellar winds. In this paper we construct a grid of quasi-static HII region models to explore how choices about these parameters alter HII regions' emission line ratios. We find that, when radiation pressure is included in our models, HII regions reach a saturation point beyond which further increases in the luminosity of the driving stars does not produce any further increase in effective ionization parameter, and thus does not yield any further alteration in an HII region's line ratio. We also show that, if stellar winds are assumed to be strong, the maximum possible ionization parameter is quite low. As a result of this effect, it is inconsistent to simultaneously assume that HII regions are wind-blown bubbles and that they have high ionization parameters; some popular HII region models suffer from this inconsistency. Our work in this paper provides a foundation for a companion paper in which we embed the model grids we compute here within a population synthesis code that enables us to compute the integrated line emission from galactic populations of HII regions.