Synthetic AGB evolution. 3: The influence of different mass-loss laws

Statistics – Computation

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Asymptotic Giant Branch Stars, Computational Astrophysics, Magellanic Clouds, Planetary Nebulae, Stellar Evolution, Stellar Luminosity, Stellar Models, Stellar Winds, Abundance, Constraints, Mass Transfer, Mathematical Models, Spectral Sensitivity

Scientific paper

In Paper 1 of this series we presented a model to calculate in a synthetic way the evolution of thermal-pulsing asymptotic giant branch (AGB) stars. The model was applied to the large magellanic cloud (LMC) and values were derived for the minimum core mass for third dredge-up and the dredge-up efficiency. In Paper 1 mass loss on the AGB was parameterized with a Reimers mass loss law with a best-fit value for the coefficient etaAGB of 5. In Paper 2 we showed that the best fitting model of Paper 1 could also reproduce the observed abundance patterns in planetary nebulae (PNe) in the LMC, under the assumption that there is no dredge-up after hot bottom burning (HBB) ceases. To investigate the sensitivity of the results in Papers 1 and 2 to the adopted mass loss law we repeat in this paper the analysis of Papers 1 and 2 for two recently proposed mass loss laws, viz. that of Vassiliadis & Wood (1993, VW) and that of Blocker 7 Schoenberner (1993, BS). We find that the BS-law with a scaling factor etaBS = 0.1 fits all observational constraints equally well as the Reimers law. For the VW-law no combination of parameters could be found that fits all constraints simultaneously. This is probably due to the extreme luminosity dependence (M(dot) approximately Lalpha, alpha = 6) implied by the VW-law. We conclude that synthetic AGB models with mass loss laws that are moderately luminosity dependent) 1 less than alpha less than or approximately 4) can be made to fit all presently available observational constraints.

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