Compulsory Deep Mixing of 3He and CNO Isotopes on the First Giant Branch

Details Compulsory Deep Mixing of 3He and CNO Isotopes on the First Giant Branch Compulsory Deep Mixing of 3He and CNO Isotopes on the First Giant Branch

Nov 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aipc..948...27e&link_type=abstract

UNSOLVED PROBLEMS IN STELLAR PHYSICS: A Conference in Honor of Douglas Gough. AIP Conference Proceedings, Volume 948, pp. 27-34

Physics

Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages, Giant And Subgiant Stars

Scientific paper

We have found a deep-mixing process which occurs during First Giant Branch (FGB) evolution. It begins at the point in evolution when the surface convection zone (SCZ), having previously grown in size, starts to shrink, and it is driven by a local minimum that develops in the mean molecular weight as a result of the burning of 3He. This mixing can solve two important observational problems. One is why the interstellar medium (ISM) has not been considerably enriched in 3He since the Big Bang. The other is why products of nucleosynthesis such as 13C are progressively enriched on the upper FGB, when classical stellar modelling says that no further enrichment should take place beyond the First Dredge-Up (FDU) episode, somewhat below the middle of the FGB.

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