A grid of synthetic ionizing spectra for very hot compact stars from NLTE model atmospheres

By T. Rauch. 2003

166 citations recorded by the source corpus.

The precise analysis of properties of planetary nebulae is strongly dependent on good models for the stellar ionizing spectrum. Observations in the UV - X-ray wavelength range as well as NLTE model atmosphere calculations of spectra of their exciting stars have shown that neither blackbody fluxes nor "standard" NLTE atmosphere models which are composed out of hydrogen and helium only are good approximations. Strong dierences between synthetic spectra from these compared to observed spectra at energies higher than 54 eV (He II ground state) can be ascribed to the neglect of metal-line blanketing. Realistic modeling of the emergent fluxes of hot stars in the UV - X-ray wavelength range requires metal-line blanketed NLTE model atmospheres which include all elements from hydrogen up to the iron-group. For this purpose, we present a grid (solar and halo abundance ratios) of metal-line blanketed NLTE model atmosphere fluxes which covers the parameter range of central stars of planetary nebulae.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

View Paper: https://www.semanticscholar.org/paper/5245c5b43c43619e15f82b3c539877b713385124

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Citations in the corpus

Stellar Population Inference with Prospector (2020, methodology): “Those libraries are supplemented with the TP-AGB library from Lançon & Wood (2000), the post-AGB library from Rauch (2003), and the WMBASIC hot star library from Eldridge et al. (2017).”
Modeling the Panchromatic Spectral Energy Distributions of Galaxies (2013, background): “At the high temperature end, i.e., Wolf-Rayet and O-type main sequence stars, the state-of-the-art libraries are from Smith, Norris & Crowther (2002) and Lanz & Hubeny (2003), while for hotter compact objects (e.g., post-AGB stars) the most up-to-date models are from Rauch (2003).”
Nebular Continuum and Line Emission in Stellar Population Synthesis Models (2016, background): “Post-asymptotic giant branch (post-AGB) stellar isochrones are from Vassiliadis & Wood (1994), with post-AGB spectra from Rauch (2003).”