![]() We also included mass loss prior to the AGB. Mass loss on the AGB is included through a Reimers Law. The effect of hot bottom burning (HBB) is included in an approximate way. ![]() The effects of first, second and third dredge-up are taken into account. Most of the relations used are metallicity dependent to be able to make a realistic comparison with stars of different metallicity. The variation of the luminosity during the interpulse period is taken into account as well as the fact that, initially, the first few pulses are not yet at full amplitude and that the luminosity is lower than given by the standard core-mass-luminosity relations. Our model is more realistic than previous synthetic evolution models in that more physics has been included. The evolution is started at the first thermal pulse (TP) and is terminated when the envelope mass has been lost due to mass loss or when the core mass reaches the Chandrasekhar mass. We have constructed a model to calculate in a synthetic way the evolution of stars on the asymptotic giant branch (AGB).
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