Volume 583, November 2015
|Number of page(s)||35|
|Section||Stellar structure and evolution|
|Published online||29 October 2015|
Three-dimensional modeling of ionized gas
II. Spectral energy distributions of massive and very massive stars in stationary and time-dependent modeling of the ionization of metals in H ii regions⋆
Institut für Astronomie und Astrophysik der Universität München, Scheinerstraße 1, 81679 München, Germany
e-mail: email@example.com, firstname.lastname@example.org, email@example.com
Received: 12 September 2014
Accepted: 9 January 2015
Context. H ii regions play a crucial role in the measurement of the chemical composition of the interstellar medium and provide fundamental data about element abundances that constrain models of galactic chemical evolution. Discrepancies that still exist between observed emission line strengths and those predicted by nebular models can be partly attributed to the spectral energy distributions (SEDs) of the sources of ionizing radiation used in the models as well as to simplifying assumptions made in nebular modeling.
Aims. One of the main influences on the nebular spectra is the metallicity, both nebular and stellar, which shows large variations even among nearby galaxies. Although nebular modeling often involves testing of different nebular metallicities against their influence on the predicted spectra, adequate grids of stellar atmospheres and realistic SEDs for different metallicities are still lacking. This is unfortunate because the influence of stellar metallicity on nebular line strength ratios, via its effect on the SEDs, is of similar importance as variations in the nebular metallicity. To overcome this deficiency we have computed a grid of model atmosphere SEDs for massive and very massive O-type stars covering a range of metallicities from significantly subsolar (0.1 Z⊙) to supersolar (2 Z⊙).
Methods. The SEDs have been computed using a state-of-the-art model atmosphere code that takes into account the attenuation of the ionizing flux by the spectral lines of all important elements and the hydrodynamics of the radiatively driven winds and their influence on the SEDs. For the assessment of the SEDs in nebular simulations we have developed a (heretofore not available) 3D radiative transfer code that includes a time-dependent treatment of the metal ionization.
Results. Using the SEDs in both 1D and 3D nebular models we explore the relative influence of stellar metallicity, gas metallicity, and inhomogeneity of the gas on the nebular ionization structure and emission line strengths. We find that stellar and gas metallicity are of similar importance for establishing the line strength ratios commonly used in nebular diagnostics, whereas inhomogeneity of the gas has only a subordinate influence on the global line emission.
Conclusions. Nebular diagnostics as a quantitative tool for measuring the abundances in the interstellar gas can be used to its full potential only when the influence of SEDs, metallicity, and geometric structure of the nebula are taken into account. For these purposes, detailed stellar SEDs like those of our grid are an essential ingredient for the photoionization models used to predict nebular emission line spectra.
Key words: radiative transfer / stars: early-type / stars: massive / stars: winds, outflows / stars: mass-loss / HII regions
Appendices are available in electronic form at http://www.aanda.org
© ESO, 2015
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