Grids of model spectra for WN stars, ready for use

By W. Hamann, G. Gräfener. 2004

155 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Computational Mechanics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/9f9bdd35b9b85ee48de85aa95279342f13704b75

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Michela Mapelli
2. S. Charlot
3. S. Smartt
4. C. Conroy
5. Daniel Schaerer
6. M. Pettini
7. G. Meynet
8. Julia Gutkin

In Computational Mechanics

1. W. Hamann
2. P. Crowther
3. G. Graefener
4. A. Liermann
5. H. Todt
6. A. Sander
7. J. Eldridge
8. G. Gräfener

In Instrumentation

1. C. Conroy
2. S. Charlot
3. M. Pettini
4. S. Smartt
5. J. Eldridge
6. Julia Gutkin
7. Michela Mapelli
8. C. Steidel

Citations in the corpus

• The Galactic WN stars. Spectral analyses with line-blanketed model atmospheres versus stellar evolut (2006, methodology): “The PoWR code was used to establish two grids of WNtype models (Hamann & Gräfener 2004).”
• A LIBRARY OF THEORETICAL ULTRAVIOLET SPECTRA OF MASSIVE, HOT STARS FOR EVOLUTIONARY SYNTHESIS (2010, background): “PoW-R and PHOENIX are not optimized for the modeling of OB-stars but rather Wolf–Rayet (W-R) and late-type stars, respectively.”
• The Wolf-Rayet stars in the Large Magellanic Cloud - A comprehensive analysis of the WN class (2014, methodology): “For more details of the PoWR code see Hamann & Gräfener (2004).”
• Physical Properties of Wolf-Rayet Stars (2006, background): “Various X-ray to mid-IR spectroscopic datasets of Galactic Wolf-Rayet stars are presented in Table 1, including extreme ultraviolet synthetic spectra from model atmospheres (Smith, Norris & Crowther 2002; Hamann & Gräfener 2004).”
• Mass loss from late-type WN stars and its Z-dependence: very massive stars approaching the Eddington limit (2008, methodology): “A large part of the galactic WN population has been re-analyzed by Hamann et al. (2006), based on a publicly accessible grid of line-blanketed atmosphere models (Hamann & Gräfener 2004, http://www.astro.physik.uni-potsdam.de).”
• The Galactic WC stars Stellar parameters from spectral analyses indicate a new evolutionary sequence (2012, methodology): “The model basics are described in Gräfener et al. (2002) and Hamann & Gräfener (2004).”
• PARSEC evolutionary tracks of massive stars up to 350 M ☉ at metallicities 0.0001 ≤ Z ≤ 0.04 (2015, methodology): “To reproduce their spectra we make use of the most recent library of WR models computed by the Potsdam group (PoWR) (Gräfener, Koesterke & Hamann 2002; Hamann & Gräfener 2003, 2004; Sander, Hamann & Todt 2012; Hamann, Gräfener & Liermann 2006; Hainich et al. 2014).”
• The death of massive stars – I. Observational constraints on the progenitors of Type II-P supernovae (2008, methodology): “We then downloaded model WR spectra from the Potsdam data base (Hamann & Gräfener 2004),16 appropriate to the temperature of each WR subtype.”
• THE EFFECTS OF STELLAR ROTATION. II. A COMPREHENSIVE SET OF STARBURST99 MODELS (2014, methodology): “Starburst99 uses the extended, expanding model atmospheres WM-Basic (Pauldrach et al. 1998), CMFGEN (Hillier & Miller 1998, 1999), and PoWR (Gräfener et al. 2002; Hamann & Gräfener 2003, 2004) for its various outputs.”
• Modelling the nebular emission from primeval to present-day star-forming galaxies (2016, background): “…libraries covering different effective-temperature, luminosity-class and wavelength ranges (Pauldrach et al. 2001; Rauch 2002; Lanz & Hubeny 2003; Hamann & Gräfener 2004; Martins et al. 2005; Rodŕıguez-Merino et al. 2005; Sánchez-Blázquez et al. 2006; MNRAS 000, 1–20 (2016) Lanz & Hubeny…”