Nucleosynthesis of solar system material in a low-mass, low-metallicity asymptotic giant branch star

Details Nucleosynthesis of solar system material in a low-mass, low-metallicity asymptotic giant branch star Nucleosynthesis of solar system material in a low-mass, low-metallicity asymptotic giant branch star

Oct 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...333l..25h&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 333, Oct. 1, 1988, p. L25-L28. Research supported by the National

Astronomy and Astrophysics

Astrophysics

95

Asymptotic Giant Branch Stars, Metallicity, Nuclear Astrophysics, Solar System, Stellar Evolution, Carbon, Helium, Neutrons, Stellar Mass

Scientific paper

This study confirms that, following a thermal pulse in a low-mass AGB star of low metallicity, the opacity in an expanding, cool, helium- und carbon-rich region is ultimately responsible for the activation of the 13C(α, n)16O neutron source; however, dredge up of processed material occurs only if overshoot is assumed. Material in the stellar interior is irradiated by neutrons, and in the models presented here lead to a neutron exposure τ ≈ 0.14 mb-1. Reprocessing of irradiated material during repeated thermal pulses provides a neutron exposure characterized by an exposure parameter τ0 ≈ 0.2 mb-1, which is remarkably similar to the exposure parameter that characterizes solar system s-process material.

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