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. 11

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Left panel: evolutionary tracks in Hertzsprung-Russell diagram of 1.5 and 2.0 Z_⊙(solid and dotted lines respectively) stars at solar metallicity. Right panel: maximal amplitude over Sun value as a function of the large separation for the same models. As in Fig. 5, the lines color indicates the evolutionary.

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