New grids of stellar models including tidal-evolution constants up to carbon burning. III. From 0.8

By A. Claret. 2004

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View Paper: https://www.semanticscholar.org/paper/b2fcb56c3881a6244c8a8101f74e51493e3e6219

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In Astronomy and Astrophysics

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The spin of the second-born black hole in coalescing binary black holes (2018, background): “Red: data from Siess et al. (2013); blue: data from Claret (2004); green: results from this study.”
A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun (2010, methodology): “For main sequence and post-main sequence stars we used evolutionary models starting from the zero-age main sequence (ZAMS) from Schaller et al. (1992), Claret (2004), Pietrinferni et al. (2004)4, Bertelli et al. (2008, 2009) and Marques et al. (2008).”
Limb and gravity-darkening coefficients for the TESS satellite at several metallicities, surface gravities, and microturbulent velocities (2016, methodology): “Therefore, the general equation which will be adopted here to compute y ( λ ) is: The e ﬀ ects of the convection on y ( λ ) are important for cooler models and ( d ln T e ﬀ / d ln g ) was computed considering the bolo-metric GDE previously calculated (see Claret (2004)).”
Homogeneous studies of transiting extrasolar planets - III. Additional planets and stellar models (2010, background): “Theoretical LD coefficients have been taken from Van Hamme (1993), Claret (2000, 2004a) and Claret & Hauschildt (2003).”
Homogeneous studies of transiting extrasolar planets – IV. Thirty systems with space-based light curves (2011, background): “As in Paper III Iuse five sets of model predictions:Claret (Claret 2004, 2005, 2006, 2007), Y2 (Demarque et al. 2004),Teramo(Pietrinferni et al. 2004),VRSS (VandenBerg et al. 2006) andDSEP(Dotter et al. 2008).”
The Adequacy of Stellar Evolution Models for the Interpretation of the Color-Magnitude Diagrams of Resolved Stellar Populations (2005, background): “We will only occasionally discuss (if at all) libraries that refer to a limited range of masses and/or metallicities (e.g., Stothers & Chin 1991; Jimenez & McDonald 1996; Baraffe et al. 1998; Ventura et al. 1998; Bono et al. 2000; Montalbán, D’Antona & Mazzitelli 2000; Claret 2004).”
Dynamical Simulations of Magnetically Channeled Line-driven Stellar Winds. I. Isothermal, Nonrotating, Radially Driven Flow (2002, background): “…constant k can be estimated from stellar structure models, and should be typically k ≈ 0.1, perhaps somewhat higher near the zero-age main sequence (ZAMS), and then decreasing by up to 50% with age (Claret 2004).2 Perhaps the most difficult parameters to infer are those for the stellar wind.”
A possible black hole in the γ-ray microquasar LS 5039 (2005, methodology): “We have estimated the synchronization time-scale of the optical component of LS 5039 using the formalism by Zahn (1989) (as formulated in Claret & Cunha 1997) and the tidal evolution parameters of the stellar models of Claret (2004).”
High-precision photometry by telescope defocussing. I. The transiting planetary system WASP-5 (2009, methodology): “We have adopted the values of the properties obtained using the Claret models, in order to retain homogeneity with the analyses of Southworth (2009).”
A REVISED AGE FOR UPPER SCORPIUS AND THE STAR FORMATION HISTORY AMONG THE F-TYPE MEMBERS OF THE SCORPIUS–CENTAURUS OB ASSOCIATION (2011, methodology): “They deconstructed the spectroscopic pair into a B1III primary with a B1V secondary with ∆V ≃ 0.80, and a system age of ∼10 Myr using the Claret (2004) evolutionary models.”