Implications of low-energy fusion hindrance on stellar burning and nucleosynthesis

Details Implications of low-energy fusion hindrance on stellar burning and nucleosynthesis Implications of low-energy fusion hindrance on stellar burning and nucleosynthesis

Sep 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007phrvc..76c5802g&link_type=abstract

Physical Review C, vol. 76, Issue 3, id. 035802

Physics

Nuclear Physics

24

Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages, Abundances, Chemical Composition, Nuclear Physics Aspects Of Novae, Supernovae, And Other Explosive Environments, Fusion And Fusion-Fission Reactions

Scientific paper

We investigate the consequences of a new phenomenological model prediction of strongly reduced low-energy astrophysical S-factors for carbon and oxygen fusion reactions on stellar burning and nucleosynthesis. The new model drastically reduces the reaction rates in stellar matter at temperatures T≲(3-10)×108 K, especially at densities ρ≳109 g cm-3, in a strongly screened or even pycnonuclear burning regime. We show that these modifications change the abundance of many isotopes in massive late-type stars and in particular strongly enhance the abundances of long-lived radioactive isotopes such as Al26 and Fe60. The reduced reaction rates also significantly complicate carbon ignition (shift carbon ignition to higher temperatures and densities) in massive accreting white dwarfs exploding as type Ia supernovae and in accreting neutron stars producing superbursts. This would require much higher ignition densities for white dwarf supernovae and would widen the gulf between theoretical and inferred ignition depths for superbursts.

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