Measurement of the Fe60(n,γ)61Fe Cross Section at Stellar Temperatures

Details Measurement of the Fe60(n,γ)61Fe Cross Section at Stellar Temperatures Measurement of the Fe60(n,γ)61Fe Cross Section at Stellar Temperatures

Apr 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009phrvl.102o1101u&link_type=abstract

Physical Review Letters, vol. 102, Issue 15, id. 151101

Physics

5

Nucleosynthesis In Late Stellar Evolution, Radiative Capture, 59<=A<=89, Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages

Scientific paper

Observations of galactic γ-ray activity have challenged the current understanding of nucleosynthesis in massive stars. Recent measurements of Fe60 abundances relative to Alg26 have underscored the need for accurate nuclear information concerning the stellar production of Fe60. In light of this motivation, a first measurement of the stellar Fe60(n,γ)Fe61 cross section, the predominant destruction mechanism of Fe60, has been performed by activation at the Karlsruhe Van de Graaff accelerator. Results show a Maxwellian averaged cross section at kT=25keV of 9.9±1.4(stat)2.8(syst)mbarn, a significant reduction in uncertainty with respect to existing theoretical discrepancies. This result will serve to significantly constrain models of Fe60 nucleosynthesis in massive stars.

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