The nucleosynthesis of heavy elements in low-mass AGB stars

Details The nucleosynthesis of heavy elements in low-mass AGB stars The nucleosynthesis of heavy elements in low-mass AGB stars

Feb 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997cha%26a..21...59w&link_type=abstract

Chinese Astronomy and Astrophysics, Volume 21, Issue 1, p. 59-69.

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

We take 13C(α,n)16O as neutron source, allow for variation of the mass of the nucleus with thermal pulse number and adopt the unbranched s process path from 56Fe to 210Bi in an attempt to explain the overabundance of heavy elements in MS and S stars. We found stars with larger masses have larger dilution factors because of a stronger convection and that these stars fall in four different regions in the abundance diagram, thus enabling a rough estimate of the mass to be made. We show that, for a 2.5 Msolar star, the third dredge-up stops after a certain number of pulses because of the formation of a hollow shell structure, so the star will show no Tc and this can account for the existence of binary systems consisting of a ``Tc-no'' AGB star with a main-sequence star companion.

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