Extended Data Fig. 2: Examples of theoretical IFMRs that fail to account for the kink in the semi-empirical IFMR.
From: Carbon star formation as seen through the non-monotonic initial–final mass relation
a, Too high efficiency of the 3DU in low-mass stars: λ = 0.5 is assumed for all models that experience the 3DU. b, Mass loss insensitive to the photospheric chemical composition: the B95 mass-loss formula is applied to all models, irrespective of the photospheric C/O. The semi-empirical IFMR is the same as in Fig. 1, with error bars covering the range of ± 1 σ.
