The ionizing radiation from massive stars and its impact on HII regions: results from modern model atmospheres

TL;DR

This study compares ionizing spectral energy distributions from four modern stellar atmosphere models for different O-type stars, analyzing their impact on nebular properties and emphasizing the importance of model choice.

Contribution

It provides a detailed comparison of modern stellar atmosphere codes' SED predictions and assesses their effects on nebular ionization and temperature structures.

Findings

Better agreement in SEDs when models are compared using the observational approach.

Significant differences at energies above 30 eV among models.

Variations in nebular ionization structures impact abundance determinations.

Abstract

We present a detailed comparison of the ionizing spectral energy distributions (SEDs) predicted by four modern stellar atmosphere codes, TLUSTY, CMFGEN, WMbasic, and FASTWIND. We consider three sets of stellar parameters representing a late O-type dwarf (O9.5 V), a mid O-type (O7 V) dwarf, and an early O-type dwarf (O5.5 V). We explore two different possibilities for such a comparison, following what we called evolutionary and observational approaches: in the evolutionary approach one compares the SEDs of stars defined by the same values of Teff and logg; in the observational approach the models to be compared do not necessarily have the same Teff and logg, but produce similar H and HeI-II optical lines. We find that there is a better agreement, in terms of Q(H0), the ratio Q(He0)/Q(H0), and the shape of the SEDs predicted by the four codes in the spectral range between 13 and 30 eV, when models are compared following the observational approach. However, even in this case, large differences are found at higher energies. We then discuss how the differences in the SEDs may affect the overall properties of surrounding nebulae in terms of temperature and ionization structure. We find that the effect over the nebular temperature is not larger than 300-350 K. Contrarily, the different SEDs produce significantly different nebular ionization structures. This will lead to important consequences on the establishment of the ionization correction factors that are used in the abundance determination of HII regions, as well as in the characterization of the ionizing stellar population from nebular line ratios.