New Grids of ATLAS9 Model Atmospheres

By F. Castelli, R. Kurucz. 2004

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New opacity distribution functions (ODFs) for several metallicities have been computed. The main improvements upon previous ODFs computed by Kurucz (1990) are: (1) the replacement of the solar abundances from Anders & Grevesse (1989) with those from Grevesse & Sauval (1998); (2) the replacement of the TiO lines provided by Kurucz (1993) with the TiO lines from Schwenke (1998), as distributed by Kurucz (1999a); (3) the addition of the H2O lines from Partridge & Schwenke (1997) as distributed by Kurucz (1999b); (4) the addition of the HI-HI and HI-H+ quasi-molecular absorptions near 1600 A and 1400 A computed according to Allard et al. (1998). Other minor improvements are related with some changes in a few atomic and molecular data. New grids of ATLAS9 model atmospheres for Teff from 3500K to 50000K and logg from 0.0 dex to 5.0 dex have been computed for several metallicities with the new ODFs. Preliminary comparisons of the results from the old and new models have shown differences in the energy distributions of stars cooler than 4500K, in the ultraviolet energy distribution of metal-poor A-type stars, in the U-B and u-b color indices for Teff<7000K and in all the color indices for Teff<4250K.

Subfields: Astronomy and Astrophysics, Atmospheric Science, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/c9f41d3243ca46b59ad24700243a4b182ed89950

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Citations in the corpus

Evolutionary stellar population synthesis with MILES – II. Scaled-solar and α-enhanced models (2015, background): “Model atmospheres from Castelli & Kurucz (2003) are adopted for effective temperatures Teff ≥ 3500 K, and from Plez (1992) for Teff 3500 K.”
NONSTEADY ACCRETION IN PROTOSTARS (2008, methodology): “The molecular, atomic, and ionized gas opacities have been calculated using the Opacity Distribution Function (ODF) method (Castelli & Kurucz 2004; Sbordone et al. 2004; Castelli 2005; Zhu et al. 2007) which is a statistical approach to handling line blanketing when millions of lines are present in…”
Measuring the rotation period distribution of field M dwarfs with Kepler (2013, methodology): “…probability maximisation (Brown et al. 2011), matching observed colours, estimated from Sloan g, r, i, z filters, 2MASS JHK, and D51 (510 nm), to the stellar atmosphere models of Castelli & Kurucz (2004), resulting in typical uncertainties of 200K for Teff and 0.5 dex for log g, respectively.”
DISEQUILIBRIUM CARBON, OXYGEN, AND NITROGEN CHEMISTRY IN THE ATMOSPHERES OF HD 189733b AND HD 209458b (2011, methodology): “…thermal structure of the planet, the planet’s metallicity and radius, or the spectrum of the host star (note that we have used the models of Castelli & Kurucz 2004 to simulate the spectrum of the host stars, with other stellar and planetary parameters as described in Torres et al. 2008).”
KEPLER ECLIPSING BINARY STARS. I. CATALOG AND PRINCIPAL CHARACTERIZATION OF 1879 ECLIPSING BINARIES IN THE FIRST DATA RELEASE (2010, methodology): “Spectral classification and stellar parameters were estimated using dedicated pre-launch ground-based optical multi-color photometry plus 2MASS J, K, H magnitudes, matched to the Castelli & Kurucz (2004) model stellar atmospheres and Girardi et al. (2000) evolutionary tracks.”
Empirical extinction coefficients for the GALEX, SDSS, 2MASS and WISE passbands (2013, methodology): “The predicted values are calculated by convolving a synthetic stellar spectral model from Castelli & Kurucz (2004) of Teff = 7000 K, log g = 4.5 and [Fe/H] = 1 without and with dust extinction of E(B − V) = 0.4.”
MEASURING REDDENING WITH SLOAN DIGITAL SKY SURVEY STELLAR SPECTRA AND RECALIBRATING SFD (2010, methodology): “We have repeated the full analysis using four different grids (Gustafsson et al. 2008; Castelli & Kurucz 2004; Lee et al. 2008a; Munari et al. 2005).”
SPITZER PHASE CURVE CONSTRAINTS FOR WASP-43b AT 3.6 AND 4.5 μm (2016, methodology): “The former requires the application of a stellar limb-darkening model, for which we adopt a quadratic equation (Claret 2000) with values derived from stellar Kurucz models (Castelli & Kurucz 2004).”
ARGOS – IV. The kinematics of the Milky Way bulge (2013, methodology): “The stellar parameters were derived from aχ2 comparison with synthetic spectra generated in the 1D Local Thermal Equilibrium (LTE) stellar synthesis program MOOG (Sneden 1973) using the Castelli/Kurucz model atmospheres (Castelli & Kurucz 2004).”
SELECTION, PRIORITIZATION, AND CHARACTERISTICS OF KEPLER TARGET STARS (2010, background): “The Castelli & Kurucz (2004) models provide flux as a function of wavelength for temperatures ranging from 3500 to 50,000 K, surface gravities of 0–5.5 dex, and metallicities of −3.5 to +0.5.”
THE OCCURRENCE RATE OF SMALL PLANETS AROUND SMALL STARS (2013, methodology): “Unlike the ATLAS9 models (Castelli & Kurucz 2004) used in development of the Kepler Input Catalog, the Dartmouth models perform well for low-mass stars because the package uses PHOENIX atmospheres to model stars cooler than 10,000K.”
A REVISED EFFECTIVE TEMPERATURE SCALE FOR THE KEPLER INPUT CATALOG (2011, methodology): “To correct for differences between the KIC and the model logg values, we used logg sensitivities of thegriz colors using Castelli & Kurucz (2004) ATLAS9 models, as described in Section 3.2.”
A TEMPERATURE AND ABUNDANCE RETRIEVAL METHOD FOR EXOPLANET ATMOSPHERES (2009, methodology): “We use a Kurucz model for the stellar spectrum (Castelli & Kurucz, 2004).”