The β-decay rates of 59Fe isotopes in shell burning environments and their influences on the production of 60Fe in massive star

Abstract

The experimental B(GT) strengths of the 59Fe excited states were employed to determine the transition strengths which greatly contribute 59Fe stellar β–decay at typical carbon shell burning temperature. The result has been compared with the theoretical rates FFN (Fuller-Fowler-Newman) and LMP (Langanke&Martinez-Pinedo). Impact of the newly determined rate on the synthesis of cosmic γ emitter 60Fe has also been studied using one-zone model calculation. Our results show 59Fe stellar β−decay rate plays an important role in the 60Fe nucleosynthesis. However the uncertainty of the decay rate is rather large due to the error of B(GT) strength that requires further studies.