The Galactic WN stars. Spectral analyses with line-blanketed model atmospheres versus stellar evolut

By W. Hamann, G. Gräfener, A. Liermann. 2006

257 citations recorded by the source corpus.

An infrared light-receiving device includes an optical absorption layer disposed on a principal surface of a substrate and an optical filter disposed on the optical absorption layer, the optical filter including first, second, and third semiconductor regions that are arranged in that order in a direction from the optical absorption layer to the optical filter, each of the first, second, and third semiconductor regions including an n-type InGaAs layer. The optical absorption layer includes a type-II superlattice structure. The first semiconductor region contains an n-type impurity with a concentration of 2.0×1019 cm−3 or more. The third semiconductor region contains an n-type impurity with a concentration of 3.0×1018 cm−3 or less and 8.0×1017 cm−3 or more. The second semiconductor region contains an n-type impurity with a concentration between the impurity concentration of the first semiconductor region and the impurity concentration of the third semiconductor region.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/613314bc7e69bc498d5e19dc7b3de434f478211c

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

In Instrumentation

Citations in the corpus

Grids of stellar models with rotation - II. WR populations and supernovae/GRB progenitors at Z = 0.014 (2012, methodology): “For this we used the sample of Galactic WN stars analysed by Hamann et al. (2006), which has 20 stars in common with our sample of nearby WR stars.”
The Galactic WC stars Stellar parameters from spectral analyses indicate a new evolutionary sequence (2012, methodology): “Thus, the “diluted emission line” (d.e.l.) criterion, whicis insufficient for WN stars as emphasized by Hamann et al. (2006), seems to work fine for WC stars when distinguishing single stars from binaries.”
Mass loss from late-type WN stars and its Z-dependence: very massive stars approaching the Eddington limit (2008, methodology): “The dichotomy among the WN subtypes, where the H-rich WNL stars show much higher luminosities than the earlier subtypes (e.g., Hamann et al. 2006), indicates that the progenitors of H-rich WNL stars are very massive stars with masses around 120M⊙.”
The Wolf-Rayet stars in the Large Magellanic Cloud - A comprehensive analysis of the WN class (2014, methodology): “The mass-loss rates of the WN stars in the LMC obtained in the present study can be compared with those of the Galactic WN stars from Hamann et al. (2006).”
Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars (2014, background): “It is suspicious that most H-poor WR stars have luminosities of log(L/L⊙)=5.5 to 5.8 (Crowther 2007, Hamann et al. 2006), which also corresponds to the strongest RSG mass loss (Fig.”
Stellar and wind properties of massive stars in the central parsec of the Galaxy (2006, background): “The luminosities of late WN stars are lower in the GC than in the sample of Hamann et al. (2006) but in good agreement with the results of Crowther et al. (1995b).”
Modelling the nebular emission from primeval to present-day star-forming galaxies (2016, background): “…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 four metallicities, 0.07Z , 0.2Z , 0.5Z and Z .”
FROM SHOCK BREAKOUT TO PEAK AND BEYOND: EXTENSIVE PANCHROMATIC OBSERVATIONS OF THE TYPE Ib SUPERNOVA 2008D ASSOCIATED WITH SWIFT X-RAY TRANSIENT 080109 (2008, background): “Their radii are in the range 1–20 R⊙ with typical sizes between 5−10 R⊙ (Herald et al. 2001; Hamann et al. 2006; Crowther 2007).”
Galaxies with Wolf-Rayet signatures in the low-redshift Universe. A survey using the Sloan Digital Sky Survey (2008, unknown): “However, the range of metallicities is limited and the spread around the relation is not established and the stellar parameters are typically hard to constrain without involving modelling (e.g. Hamann et al. 2006).”
SN 2006gy: Discovery of the Most Luminous Supernova Ever Recorded, Powered by the Death of an Extremely Massive Star like η Carinae (2006, result): “This range of mass-loss rates is in good agreement with observed values in luminous H-rich WN stars (e.g., Hamann et al. 2006) or quiescent nonoutburst LBVs (Smith et al. 2004).”
The death of massive stars – I. Observational constraints on the progenitors of Type II-P supernovae (2008, methodology): “9, we compare the locations predicted for our single-star and binary population in the Hertzsprung–Russell (HR) diagram to those inferred from the Potsdam models for observed WR stars in Hamann et al. (2006) and Sander et al. (2012).”
Fundamental properties of core-collapse Supernova and GRB progenitors: predicting the look of massive stars before death (2013, methodology): “More recently, Eldridge et al. (2013) employed atmospheric models of WR stars from the Potsdam group (Hamann et al. 2006; Sander et al. 2012) that were computed for a range of physical parameters, but not self-consistently with the evolutionary calculations.”