CESAM: a free code for stellar evolution calculations

By P. Morel, Y. Lebreton. 2008

151 citations recorded by the source corpus.

Abstract The cesam code is a consistent set of programs and routines which perform calculations of 1D quasi-hydrostatic stellar evolution including microscopic diffusion of chemical species and diffusion of angular momentum. The solution of the quasi-static equilibrium is performed by a collocation method based on piecewise polynomials approximations projected on a B-spline basis; that allows stable and robust calculations, and the exact restitution of the solution, not only at grid points, even for the discontinuous variables. Other advantages are the monitoring by only one parameter of the accuracy and its improvement by super-convergence. An automatic mesh refinement has been designed for adjusting the localisations of grid points according to the changes of unknowns. For standard models, the evolution of the chemical composition is solved by stiffly stable schemes of orders up to four; in the convection zones mixing and evolution of chemical are simultaneous. The solution of the diffusion equation employs the Galerkin finite elements scheme; the mixing of chemicals is then performed by a strong turbulent diffusion. A precise restoration of the atmosphere is allowed for.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/50501789d693d9fd2e2fb156b4391462058e8829

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In Astronomy and Astrophysics

1. D. Huber
2. D. Stello
3. W. Chaplin
4. T. Bedding
5. B. Mosser
6. A. Miglio
7. S. Hekker
8. Y. Elsworth

In Instrumentation

1. D. Huber
2. D. Stello
3. W. Chaplin
4. B. Mosser
5. T. Bedding
6. A. Miglio
7. S. Hekker
8. Y. Elsworth

Citations in the corpus

• Probing the core structure and evolution of red giants using gravity-dominated mixed modes observed with Kepler (2012, methodology): “These models were obtained using the stellar evolution code CESAM2k (Morel & Lebreton 2008), assuming a gray Eddington approximation and the435 Böhm-Vitense mixing-length formalism for convection with a mixing-length parameter α = 1.6.”
• The underlying physical meaning of the νmax νc relation (2011, methodology): “The grid is obtained by using the s ellar evolution code CESAM2k (Morel 1997; Morel & Lebreton 2008).”
• FUNDAMENTAL PROPERTIES OF STARS USING ASTEROSEISMOLOGY FROM KEPLER AND CoRoT AND INTERFEROMETRY FROM THE CHARA ARRAY (2012, methodology): “To test this, we have computed additional tracks using the 1D stellar evolution code CESAM (Morel & Lebreton 2008).”
• MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA) (2010, background): “…example, the participants (Christensen-Dalsgaard 2008; Degl’Innocenti et al. 2008; Demarque et al. 2008; Eggenberger et al. 2008; Hui-Bon-Hoa 2008; Morel & Lebreton 2008; Roxburgh 2008; Scuflaire et al. 2008; Ventura et al. 2008; Weiss & Schlattl 2008) in the CoRot Evolution and Seismic Tools…”
• Seismic diagnostics for transport of angular momentum in stars. I. Rotational splittings from the pre-main sequence to the red-giant branch. (2012, methodology): “The CESAM2K code (Morel 1997; Morel & Lebreton 2008) belongs to the second category above.”
• Gaia FGK benchmark stars: Effective temperatures and surface gravities (2015, methodology): “For several stars, detailed investigations of the evolutionary state have been done with the CESAM2k code (Morel 1997; Morel & Lebreton 2008), taking seismic data into account when available.”