Stellar krypton cross sections at kT=25 and 52 keV

Details Stellar krypton cross sections at kT=25 and 52 keV Stellar krypton cross sections at kT=25 and 52 keV

Mar 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987phrvc..35..936k&link_type=abstract

Physical Review C (Nuclear Physics), Volume 35, Issue 3, March 1987, pp.936-941

Physics

Nuclear Physics

22

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

Scientific paper

Studies of neutron capture nucleosynthesis in the s process usually refer to a thermal energy of kT=30 keV, corresponding to a temperature of T=3.5×108 K. This convention is justified as stellar neutron capture rates are in general not sensitive to temperature because of the approximate En-1/2 dependence of most capture cross sections. But several important exceptions of this rule require more detailed information on the variation of the average stellar cross section with temperature. We show that activation measurements can be performed in a quasistellar neutron spectrum for kT=52 keV, using kinematically collimated neutrons from the 3H(p,n) reaction. Neutron capture cross sections were measured in this spectrum and at kT=25 keV for 86Kr(n,γ) and for the reaction 84Kr(n,γ) 85Krm, which populates the isomeric state in 85Kr. In this way, the respective 30 keV cross sections of 3.5+/-0.3 and 16.7+/-1.2 mb could be derived by interpolation.

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