Radiation-driven winds of hot luminous stars - XIII. A description of NLTE line blocking and blanketing towards realistic models for expanding atmospheres

By A. Pauldrach, T. Hoffmann, M. Lennon. 2001

390 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics

View Paper: https://www.semanticscholar.org/paper/4e8e5509b95afc021bcb5bebaa675c449f127739

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In Astronomy and Astrophysics

1. P. Hopkins
2. C. Conroy
3. R. Dav'e
4. L. Hernquist
5. Lisa J. Kewley
6. N. Smith
7. C. Faucher-Giguére
8. R. Somerville

In Atomic and Molecular Physics, and Optics

1. D. John Hillier
2. T. Lanz
3. J. Bouret
4. D. Massa
5. A. Sternberg
6. Tadziu Hoffman
7. A. Pauldrach
8. I. Hubeny

Citations in the corpus

• Line-driven Winds, Ionizing Fluxes, and Ultraviolet Spectra of Hot Stars at Extremely Low Metallicity. I. Very Massive O Stars (2002, methodology): “…at the ionization frequency calculated from line-blanketed unified NLTE model atmospheres with spherical extension and stellar winds (see Pauldrach et al. 1998, 2001), and W the geometrical dilution factor of the radiation field (adopted to be 13 at the base of the wind around the…”
• Realistic ionizing fluxes for young stellar populations from 0.05 to 2 Z (2002, methodology): “A total of 230 expanding, non-LTE, line-blanketed model atmospheres have been calculated for five metallicities (0.05, 0.2, 0.4, 1 and 2Z⊙) using the WM-basic code of Pauldrach et al. (2001) for O stars and the cmfgen code of Hillier & Miller (1998) for W-R stars.”
• The Physical Properties and Effective Temperature Scale of O-Type Stars as a Function of Metallicity. II. Analysis of 20 More Magellanic Cloud Stars and Results from the Complete Sample (2005, background): “…have relied solely on the ultraviolet region for modeling (see, for example, Martins et al. 2004, Garcia & Bianchi 2004, Bianchi & Garcia 2002, Pauldrach et al. 2001), while other recent studies have included both the optical and ultraviolet regions in their modeling efforts (for instance,…”
• Atmospheric NLTE-models for the spectroscopic analysis of blue stars with winds. II. Line-blanketed models (2004, methodology): “…atmospheres and synthetic spectra for massive stars including winds), namely phoenix (Hauschildt 1992), cmfgen (Hillier & Miller 1998), WM-basic (Pauldrach et al. 2001), and PoWR (Gräfener et al. 2002, Sander et al. 2015), where all of them (except for WM-basic, which uses a Sobolev…”
• A Grid of Non-LTE Line-blanketed Model Atmospheres of O-Type Stars (2002, result): “We have also compared our results to values derived from NLTE, line-blanketed, expanding model atmospheres, calculated with program WM-BASIC (Pauldrach et al. 2001).”
• Quantitative Spectroscopy of O Stars at Low Metallicity: O Dwarfs in NGC 346 (2003, methodology): “…see Hubeny, Mihalas, & Werner 2003), and several computer programs that can handle this problem are available now: CMFGEN (Hillier & Miller 1998), PHOENIX (Hauschildt, Baron, & Allard 1997), Munich programs (Pauldrach et al. 2001), and the Kiel-Potsdam code (Koesterke, Hamann, &Graefener 2002).”
• Ionizing Photon Emission Rates from O- and Early B-Type Stars and Clusters (2003, methodology): “Our " realistic " NLTE radiation-driven wind atmosphere models provide excellent matches to directly observable far-UV stellar SEDs longward of the Lyman limit (e.g., Pauldrach et al. 2001).”
• EXTRAGALACTIC CHEMICAL ABUNDANCES: DO H ii REGIONS AND YOUNG STARS TELL THE SAME STORY? THE CASE OF THE SPIRAL GALAXY NGC 300 (2009, background): “…need for a sophisticated NLTE treatment of the physical processes involving millions of metal lines in expanding atmospheres (Hillier & Miller 1998; Pauldrach et al. 2001; Puls et al. 2005), and the requirement for telescopes with large collecting areas to secure spectra of individual stars…”
• THEORETICAL EVOLUTION OF OPTICAL STRONG LINES ACROSS COSMIC TIME (2013, methodology): “We use the Pauldrach/Hillier model atmospheres, which employ the WMBASIC wind models of Pauldrach et al. (2001) for younger ages when O stars dominate the luminosity (< 3 Myr), and the CMFGEN atmospheres from Hillier & Miller (1998) for later ages when WolfRayet (W-R) stars dominate.”
• Nebular Continuum and Line Emission in Stellar Population Synthesis Models (2016, methodology): “The STARBURST-99 models adopt similar ingredients, including the same high mass-loss rate evolutionary tracks from the Geneva group, described in Meynet & Maeder (2000), the BaSeL spectral library (STARBURST-99 uses an earlier compilation, presented in Lejeune et al. 1997), and the same spectral lib”
• A LIBRARY OF THEORETICAL ULTRAVIOLET SPECTRA OF MASSIVE, HOT STARS FOR EVOLUTIONARY SYNTHESIS (2010, methodology): “Most importantly, inclusion of wind structure and X-ray ionization in the wind provides a much more realistic treatment of the radiative transfer and the associated hydrodynamics in the WM-Basic model atmosphere code (Pauldrach et al. 2001).”
• The impact of the nitrogen-to-oxygen ratio on ionized nebula diagnostics based on [N ii] emission lines (2009, neutral): “WM-Basic (version 2.11 ⋆, Pauldrach et al., 2001).”
• (Star)bursts of FIRE: observational signatures of bursty star formation in galaxies (2015, background): “…are treated as in STARBURST99 (Leitherer et al. 1999; Vázquez & Leitherer 2005; Leitherer et al. 2010, 2014), in which OB star atmospheres are from Pauldrach et al. (2001), Wolf-Rayet star atmospheres are from Hillier & Miller (1998), and all other stellar atmospheres are from Lejeune et al.…”
• Bright OB stars in the Galaxy. III. Constraints on the radial stratification of the clumping factor (2006, background): “Note that these grids have been calculated without the inclusion of X-rays; the influence of X-rays on the occupation numbers and IR/radio opacities of hydrogen is negligible (e.g., Pauldrach et al. 2001), whilst their effect on helium (through their EUV tail) has not been investigated in detail.”
• THE ORIGIN AND OPTICAL DEPTH OF IONIZING RADIATION IN THE “GREEN PEA” GALAXIES (2013, methodology): “The grids use WMBasic stellar atmosphere models (Pauldrach et al. 2001) for the O stars and CMFGEN models (Hillier & Miller 1998) for the WR stars.”
• Mass loss from hot massive stars (2008, methodology): “, these numbers are consistent with the alternative explanation in terms of a strong oxygen depletion (factor 50) in early O stars, suggested by Pauldrach et al (2001) as a result of analyses usinghomogeneousmodels.”
• O stars with weak winds: the Galactic case (2005, background): “Indeed, the main wind line profiles were not modified (see also MacFarlane et al. 1994, Pauldrach et al. 1994, 2001), indicating that X-rays are not crucial for the modelling of these lines in such high density winds.”