Thermohaline instability and rotation-induced mixing - III. Grid of stellar models and asymptotic asteroseismic quantities from the pre-main sequence up to the AGB for low- and intermediate-mass stars of various metallicities

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This article has an erratum: [https://doi.org/10.1051/0004-6361/201118331e]

Fig. 10

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From top to bottom: evolution of global stellar properties (luminosity L, effective temperature T_eff and total stellar mass M) and asteroseismic parameters (Δν, and ν_max, A_max/A_max, ⊙) on the TP-AGB of the [2.0 M_⊙, Z_⊙] model computed with rotation up to the RGB tip and thermohaline mixing all along the evolution. The abscissa is the time since the first thermal pulse.

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