Astrophysical S( E) factor of8Li (α, n 0)11B and inhomogeneous Big Bang nucleosynthesis

Details Astrophysical S( E) factor of8Li (α, n 0)11B and inhomogeneous Big Bang nucleosynthesis Astrophysical S( E) factor of8Li (α, n 0)11B and inhomogeneous Big Bang nucleosynthesis

Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990zphya.337..211p&link_type=abstract

Zeitschrift für Physik A Atomic Nuclei, Volume 337, Issue 2, pp.211-220

Astronomy and Astrophysics

Astrophysics

24

24.30, 25.90

Scientific paper

The cross section of the11B( n, α)8Li reaction has been measured at E n=7.6 to 12.6 MeV. The neutron beam was produced via the D( d, n)3He reaction and a BF 3 counter (with natural B isotopic composition) served both as target for the11B nuclides and as detector for the observation of the delayed α-activity of8Li. The data match well with previous results obtained at E n =12.5 to 20.0 MeV. Using the principle of detailed balance the data were converted to the case of the8Li( α, n 0)11B reaction. The associated astrophysical S( E) factor is dominated by a resonance at E R=0.58 MeV of width Γ R =200 keV, with S( E R )=8400 MeV b. This S (E R ) value for the n0 channel alone is already three times higher than the constant S( E) factor assumed previously and, thus, strengthens the significance of inhomogeneous Big Bang nucleosynthesis.

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