Importance of (n,p) reactions for stellar beta decay rates

Details Importance of (n,p) reactions for stellar beta decay rates Importance of (n,p) reactions for stellar beta decay rates

Jun 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996phrvc..53.3139a&link_type=abstract

Physical Review C (Nuclear Physics), Volume 53, Issue 6, June 1996, pp.3139-3142

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Nucleosynthesis In Novae, Supernovae, And Other Explosive Environments, Relation With Nuclear Matrix Elements And Nuclear Structure, Charge-Exchange Reactions, 39<=A<=58

Scientific paper

Recent (n,p) experiments on 54Fe, 56Fe, 58Ni, and 59Co have measured Gamow-Teller resonances which are crucial for determining stellar beta decay rates in 54Mn, 56Mn, 58Co, and 59Fe, respectively. These nuclei are important players in the iron-core URCA process, which is a dynamic balancing of electron capture and beta decay rates during the final stage of nuclear burning in massive stars. We find that three of the nuclei, after calibration from (n,p) measurements, have significantly stronger decay rates than currently expected. These stronger rates will cause a more vigorous URCA process, resulting in presupernova cores which are cooler and less neutron rich than is presently used in core collapse calculations.

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