Thermohaline instability and rotation-induced mixing - I. Low- and intermediate-mass solar metallicity stars up to the end of the AGB

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

Fig. 5

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1.25 M_⊙ model with thermohaline mixing (no rotation) at the evolution point C_1.25 – (top) Lifetime of ³He, ⁷Li, ⁷Be, and ¹²C, and convective and thermohaline diffusive timescales (in years). The transition between the convective envelope and the radiative region occurs at δM = 1. (Bottom) Abundance profiles (in mass fraction) of relevant species in the same region.

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