Cesam2k20: A code for a new generation of stellar evolution models - I. Description of the code

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Volume 704 (December 2025)

A&A, 704 (2025) A79

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Table 4

Summary of mass-loss recipes available in Cesam2k20.


Name	Comments	Can be used with
pert_ext	Constant mass-loss (or gain).	Always
`pert_vink`	Mass-loss depending on L, M, T_eff, Z and terminal velocity of the wind v_∞ (Vink et al. 2001). A specific formulation for the bistability jump is also implemented.	Hot stars (T_eff > 10⁴ K)
`pert_Reimers`	Mass-loss proportional to LR/M (Reimers 1975; Maeder & Meynet 1989). Proportionality factor is calibrated on observations, but slightly varies with stellar mass and evolution stage.	Solar-type, SG, RGB, AGB, supergiants
`pert_vanLoon`	Mass-loss depending on L and T_eff for oxygen-rich and pulsating AGB and red supergiant stars (van Loon et al. 2005).	SG, RGB, AGB, supergiants
`pert_SC05`	Improved Reimers-like law, physically grounded (Schröder & Cuntz 2005). Two more quantities are involved in the expression of the mass-loss: T_eff and the gravity. Such an expression better reproduces observed mass-loss rates, in particular mass-loss rates of supergiants. The proportionality factor varies much less from one star to the other that in Reimers (1975)’s original formulation.	SG, RGB, AGB, supergiants
`pert_Rosenf14`	Rosenfield et al. (2014) improves the work of Schröder & Cuntz (2005) with a better agreement with evolved stars (TP-AGB stars which experience a series of He-shell flashes).	AGB, supergiants

Notes. They can be set to the options nom_pertm, nom_pertm_solar, nom_pertm_rgb, nom_pertm_agb, nom_pertm_hot, depending on the star type or evolutionary stage.

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