Line-blanketed model atmospheres for WR stars

By G. Gräfener, L. Koesterke, W. Hamann. 2002

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In Astronomy and Astrophysics

Citations in the corpus

Grids of model spectra for WN stars, ready for use (2004, methodology): “Details of our line-blanketing formalism are given in Gräfener et al. (2002).”
Atmospheric NLTE-models for the spectroscopic analysis of blue stars with winds. II. Line-blanketed models (2004, background): “To cure these problems, and to allow for applications that have not been possible for fastwind until to date, we have im- Article number, page 2 of 30 proved our approach by performing a precise comoving-frame radiative transfer for the complete spectrum (as done, for example, in cmfgen, PoWR, and p”
THE EFFECTS OF STELLAR ROTATION. II. A COMPREHENSIVE SET OF STARBURST99 MODELS (2014, methodology): “Currently there are no very metal-poor PoWR spectra available, and we used the solar models for all simulations presented in this paper.”
Mass loss from hot massive stars (2008, background): “This “missing” correlation is the central topic of an interesting kinematical investigation by Hamann et al (2001), who stressed the fact that the low drift rate is not a consequence of the CIRs themselves.”
THE YELLOW SUPERGIANT PROGENITOR OF THE TYPE II SUPERNOVA 2011dh IN M51 (2011, methodology): “The possibility of the progenitor source being a cluster is rejected, on the basis of: 1) the source is not spatially extended; 2) the absence of excess Hα emission; and 3) the poor fit to synthetic cluster SEDs.”
The Galactic WN stars. Spectral analyses with line-blanketed model atmospheres versus stellar evolut (2006, methodology): “The line-blanketed version of the Send offprint requests to: W.-R. Hamann e-mail:wrh@astro.physik.uni-potsdam.de Potsdam Wolf-Rayet (PoWR) model atmosphere code became available with Gräfener et al. (2002).”
The Wolf-Rayet stars in the Large Magellanic Cloud - A comprehensive analysis of the WN class (2014, methodology): “The models are calculated using complex atomic data of H, He, C, and N. Iron group elements are considered in the “superlevel approach” that encompasses ∼ 107 line transitions between ∼ 105 levels within 72 superlevels (Gräfener et al. 2002).”
Modelling the nebular emission from primeval to present-day star-forming galaxies (2016, background): “…Wolf-Rayet stars, the spectra come from the library of line-blanketed, non-LTE, spherically expanding models of Hamann & Gräfener (2004, see also Gräfener et al. 2002; Hamann & Gräfener 2003; Hamann et al. 2006; Sander et al. 2012; Hainich et al. 2014, 2015; Todt et al. 2015),1 available at…”
Mass loss from late-type WN stars and its Z-dependence: very massive stars approaching the Eddington limit (2008, methodology): “…of Fe-group transitions in non-LTE (for details ofthe numeric treatment see Koesterke et al. 1992; Hamann et al. 1992; Leuenhagen & Hamann 1994; Koesterke & Hamann 1995; Leuenhagen et al. 1996; Hamann & Koesterke 1998a; Koesterke et al. 2002; Gräfener et al. 2002; Hamann & Gräfener 2003).”
The Galactic WC stars Stellar parameters from spectral analyses indicate a new evolutionary sequence (2012, methodology): “With the inclusion of iron line blanketing and microclumping (Hillier & Miller 1999; Gräfener et al. 2002), a new generation of models have allowed better spectral fits, and led to a revision of the empirical stellar parameters.”
Stellar and wind properties of LMC WC4 stars A metallicity dependence for Wolf-Rayet mass-loss rates ? (2002, methodology): “External errors are difficult to quantify, but from test calculations carried out using the line blanketed code of Gräfener et al. (2002) the degree of consistency is excellent.”