Precise measurement of the thermal and stellar ${}^{54}$Fe($n,\gamma$)${}^{55}$Fe cross sections via AMS

Abstract

The detection of long-lived radionuclides through ultra-sensitive single atom counting via accelerator mass spectrometry (AMS) offers opportunities for precise measurements of neutron capture cross sections, e.g. for nuclear astrophysics. The technique represents a truly complementary approach, completely independent of previous experimental methods. The potential of this technique is highlighted at the example of the ${}^{54}$Fe($n,\gamma$)${}^{55}$Fe reaction. Following a series of irradiations with neutrons from cold and thermal to keV energies, the produced long-lived ${}^{55}$Fe nuclei ($t_{1/2}=2.744(9)$ yr) were analyzed at the Vienna Environmental Research Accelerator (VERA). A reproducibility of about 1% could be achieved for the detection of ${}^{55}$Fe, yielding cross section uncertainties of less than 3%. Thus, the new data can serve as anchor points to time-of-flight experiments. We report significantly improved neutron capture cross sections at thermal energy (${\sigma }_{th}=2.30\pm 0.07$ b) as well as for a quasi-Maxwellian spectrum of $kT=25$ keV ($\sigma =30.3\pm 1.2$ mb) and for $E_n=481\pm 53$ keV ($\sigma =6.01\pm 0.23$ mb). The new experimental cross sections have been used to deduce improved Maxwellian average cross sections in the temperature regime of the common $s$-process scenarios. The astrophysical impact is discussed using stellar models for low-mass AGB stars.

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Cited by in corpus (6)

• The activation method for cross section measurements in nuclear astrophysics
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• The Status and Future of Direct Nuclear Reaction Measurements for Stellar Burning
• Advances and new ideas for neutron-capture astrophysics experiments at CERN n_TOF
• Astrophysical reaction rates with realistic nuclear level densities
• Stellar ${\beta }^{-}$-decay rate of ${}^{63}$Ni and its impact on the $s$-process nucleosynthesis in massive stars