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Astron. Astrophys. Suppl. Ser.
Volume 123, Number 2, June_I 1997
Page(s) 305 - 328
DOI: 10.1051/aas:1997162

A&A Supplement series, Vol. 123, June I 1997, 305-328

Received July 29; accepted September 25, 1996

New theoretical yields of intermediate mass stars

L.B.  van den Hoektex2html_wrap592 and M.A.T.  Groenewegentex2html_wrap594

Send offprint request: L.B. van den Hoek(

tex2html_wrap596  Astronomical Institute ``Anton Pannekoek'', Kruislaan 403, NL 1098 SJ Amsterdam, The Netherlands
tex2html_wrap598  Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Straße 1, D-85748 Garching, Germany


We present theoretical yields of H, tex2html_wrap_inline554He, tex2html_wrap_inline556C, tex2html_wrap_inline558C, tex2html_wrap_inline560N, and tex2html_wrap_inline562O for stars with initial masses between 0.8 and 8 tex2html_wrap_inline564 and initial metallicities Z = 0.001, 0.004, 0.008, 0.02, and 0.04. We use the evolutionary tracks of the Geneva group up to the early asymptotic giant branch (AGB) in combination with a synthetic thermal-pulsing AGB evolution model to follow in detail the chemical evolution and mass loss up to the end of the AGB including the first, second, and third dredge-up phases. Most of the relations used are metallicity dependent to make a realistic comparison with stars of different initial abundances. The effect of Hot Bottom Burning (HBB) is included in an approximate way.

The free parameters in our calculations are the mass loss scaling parameter tex2html_wrap_inline568 for stars on the AGB (using a Reimers law), the minimum core mass for dredge-up tex2html_wrap_inline570, and the third dredge-up efficiency tex2html_wrap_inline572. As derived from previous extensive modeling, tex2html_wrap_inline574 = 4, tex2html_wrap_inline576 = 0.58 tex2html_wrap_inline578, and tex2html_wrap_inline580 including HBB are in best agreement with observations of AGB stars both in the Galactic disk and Magellanic Clouds.

The influence of specific model assumptions and adopted parameter values on the resulting AGB yields is examined and compared with earlier theoretical work. We compare the abundances predicted during the final stages of the AGB with those observed in planetary nebulae in the Galactic disk and show that the model with the aforementioned parameters is in good agreement with the observations. The metallicity dependent yields of intermediate mass stars presented in this paper are well suited for use in galactic chemical evolution models.

keywords: stars: abundances, evolution, AGB -- ISM: abundances -- galaxies: abundances

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