Stellar Atmosphere Modeling

By L. Chevallier. 2004

181 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/3d357be39adc84194f8e097fde7a215785f41b8f

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Citations in the corpus

Atomic and Molecular Opacities for Brown Dwarf and Giant Planet Atmospheres (2006, methodology): “…et al. (1997) with that from Borysow et al. (2003), it is seen that the coverage of the lower range overlaps with the data from Borysow et al. (2003) but includes a large gap in coverage centered at about 5850 cm 1, corresponding to a peak in the opacity in the data from Borysow et al. (2003).”
Advanced Forward Modeling and Inversion of Stokes Profiles Resulting from the Joint Action of the Hanle and Zeeman Effects (2008, methodology): “The most general case, where the properties of the slab vary along the ray path, has to be solved numerically.”
First stars VII - Lithium in extremely metal poor dwarfs (2006, methodology): “Our analysis used OSMARCS model atmospheres (Gustafsson et al. 1975; Plez et al. 1992; Edvardsson et al. 1993; Asplund et al. 1997; Gustafsson et al. 2003) and the turbospectrum spectral synthesis code (Alvarez & Plez 1998).”
ExoMol: molecular line lists for exoplanet and other atmospheres (2012, background): “…dogged studies of the impact of comet ShoemakerLevy 9 with Jupiter (Dinelli et al. 1997), and also the interpretation of spectra of brown dwarfs (Homeier et al. 2003), where the desperate resort of modelling them using methane spectra taken from solar system gas giants and Titan has been used…”
Lower mass loss rates in O-type stars: Spectral signatures of dense clumps in the wind of two Galactic O4 stars (2004, background): “…model atmospheres, which consistently account for the stellar wind, for departures from the Local Thermodynamic Equilibrium (LTE), and for metal line blanketing (Hubeny & Lanz 1995; Hillier & Miller 1998; Hauschildt et al. 1997; Pauldrach et al. 2001; Koesterke et al. 2002; Hubeny et al. 2003).”
First stars VI - Abundances of C, N, O, Li, and mixing in extremely metal-poor giants. Galactic evolution of the light elements (2004, methodology): “As described in Paper V, we carried out a classical LTE analysis using OSMARCS model atmospheres (Gustafsson et al. 1975; Plez et al. 1992; Edvardsson et al. 1993; Asplund et al. 1997; Gustafsson et al. 2003).”