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Parameterising the Third Dredge-up in Asymptotic Giant Branch Stars

Published online by Cambridge University Press:  05 March 2013

A. I. Karakas ,
J. C. Lattanzio  and
O. R. Pols
A. I. Karakas*
Affiliation:
School of Mathematical Sciences, Monash University, Wellington Rd, Clayton 3800, Australia
J. C. Lattanzio
Affiliation:
School of Mathematical Sciences, Monash University, Wellington Rd, Clayton 3800, Australia
O. R. Pols
Affiliation:
School of Mathematical Sciences, Monash University, Wellington Rd, Clayton 3800, Australia Astronomical Institute Utrecht, Postbus 80000, 3508 TA Utrecht, The Netherlands
*
amanda.karakas@maths.monash.edu.au
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Abstract

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We present new evolutionary sequences for low and intermediate mass stars (1−6M⊙) for three different metallicities, Z = 0.02, 0.008, and 0.004. We evolve the models from the pre-main sequence to the thermally-pulsing asymptotic giant branch phase. We have two sequences of models for each mass, one which includes mass loss and one without mass loss. Typically 20 or more pulses have been followed for each model, allowing us to calculate the third dredge-up parameter for each case. Using the results from this large and homogeneous set of models, we present an approximate fit for the core mass at the first thermal pulse, Mc1, as well as for the third dredge-up efficiency parameter, λ, and the core mass at the first dredge-up episode, Mcmin, as a function of metallicity and total mass. We also examine the effect of a reduced envelope mass on the value of λ.

Keywords

stars: AGB and post-AGBstars: evolutionstars: interiorsstars: low mass
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 19 , Issue 4 , 2002 , pp. 515 - 526
Copyright
Copyright © Astronomical Society of Australia 2002

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