Radiative C-13 burning in asymptotic giant branch stars and s-processing

Details Radiative C-13 burning in asymptotic giant branch stars and s-processing Radiative C-13 burning in asymptotic giant branch stars and s-processing

Feb 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...440l..85s&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 440, no. 2, p. L85-L87

Astronomy and Astrophysics

Astrophysics

175

Asymptotic Giant Branch Stars, Carbon 13, Nuclear Fusion, Radiative Heat Transfer, Stellar Evolution, Stellar Models, Neutron Irradiation, Stellar Convection

Scientific paper

We present new evolutionary calculations for a 3 solar mass of Population I starting from zero-age main sequence and followed up to the 25th thermal pulse of the asymptotic giant branch. The third dredge-up is found to occur in a self-consistent way from the 14th pulse on. We show that any amount of C-13 possibly synthesized at the H/He interface during the interpulse period is completely burnt through (alpha, n) reactions before the next pulse develops. As a consequence, s-elements are produced in a radiative environment, at a neutron density of at most a few 107 n/cc. There are then engulfed and diluted into the next convective pulse, where a second (minor) neutron burst occurs, driven by the (22) Ne (alpha, n) (25) Mg reaction marginally activated near the end of the He-shell instability. Despite the differences of the present model with respect to past calculations, we predict s-process distributions very close to those computed by allowing C-13 to burn in convective pulses: C-13 burning and the ensuing s-processing are confirmed to account for the main observational and experimental constraints. The reasons for this are briefly discussed. Since no C-13 survives the interpulse phase, we conclude that no modifications of the pulse shape due to the energy feedback from the (13) C (alpha, n) (16) O reaction occur.

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