Engineering topics
Linhardt, L. E.
Publications and source records attributed to Linhardt, L. E..
Measurement of 17 F(d,n) 18 Ne and the impact on the 17 F(p,γ) 18 Ne reaction rate for astrophysics
The 17 F(d,n) 18 Ne reaction is part of the astrophysical “hot CNO” cycles that are important in astrophysical environments like novae. Here, its thermal reaction rate is small owing to the relatively high energy of the resonances and therefore is dominated by direct, non-resonant capture in stellar environments at temperatures below 0.4 GK.
ANASEN: The array for nuclear astrophysics and structure with exotic nuclei
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γ spectroscopy of states in Cl 32 relevant for the S 31 ( p , γ ) Cl 32 reaction rate
Background: The 31 S(p,gamma) 32 Cl reaction becomes important for sulfur production in novae if the P-31(p, alpha)Si-28 reaction rate is somewhat greater than currently accepted. The rate of the S-31(p,gamma) Cl-32 reaction is uncertain, primarily due to the properties of resonances at E-c.m. = 156 and 549 keV. Purpose: We precisely determined the excitation energies of states in Cl-32 through high-resolution. spectroscopy including the two states most important for the S-31(p,gamma) Cl-32 reaction at nova temperatures. Method: Excited states in Cl-32 were populated using the B-10(Mg-24, 2n) Cl-32 reaction with a Mg-24 beam from the ATLAS facility at Argonne National Laboratory. The reaction channel of interest was selected using recoils in the Fragment Mass Analyzer, and we determined precise level energies by detecting. rays with Gammasphere. Results: We also observed. rays from the decay of six excited states in Cl-32. The excitation energies for two unbound levels at E-x = 1738.1 (6) keV and 2130.5 (10) keV were determined and found to be in agreement with a previous high-precision measurement of the S-32(He-3, t) Cl-32 reaction [1]. Conclusions: An updated 31 S(p,gamma) Cl-32 reaction rate is presented. With the excitation energies of important levels firmly established, the dominant uncertainty in the reaction rate at nova temperatures is due to the strength of the resonance corresponding to the 2131-keV state in Cl-32.
Particle decay of proton-unbound levels in N 12
Transfer reactions are a useful tool for studying nuclear structure, particularly in the regime of low level densities and strong single-particle strengths. Additionally, transfer reactions can populate levels above particle decay thresholds, allowing for the possibility of studying the subsequent decays and furthering our understanding of the nuclei being probed. In particular, the decay of loosely bound nuclei such as 12 N can help inform and improve structure models.The purpose of this paper is to learn about the decay of excited states in 12 N , to more generally inform nuclear structure models, particularly in the case of particle-unbound levels in low-mass systems which are within the reach of state-of-the-art ab initio calculations.
Experimental Investigation of the 19 Ne(p,γ) 20 Na Reaction Rate and Implications for Breakout from the Hot CNO Cycle
The 19 Ne(p,γ) 20 Na reaction is the second step of a reaction chain which breaks out from the hot CNO cycle, following the 15 O(α,γ) 19 Ne reaction at the onset of x-ray burst events. We investigate the spectrum of the lowest proton-unbound states in 20 Na in an effort to resolve contradictions in spin-parity assignments and extract reliable information about the thermal reaction rate. Here, the proton-transfer reaction 19 Ne(d,n) 20 Na is measured with a beam of the radioactive isotope 19 Ne at an energy around the Coulomb barrier and in inverse kinematics. We observe three proton resonances with the 19 Ne ground state, at 0.44, 0.66, and 0.82 MeV c.m. energies, which are assigned 3 + , 1 + , and (0 + ), respectively. In addition, we identify two resonances with the first excited state in 19 Ne, one at 0.20 MeV and one, tentatively, at 0.54 MeV. These observations allow us for the first time to experimentally quantify the astrophysical reaction rate on an excited nuclear state. Our experiment shows an efficient path for thermal proton capture in 19 Ne(p,γ) 20 Na, which proceeds through ground state and excited-state capture in almost equal parts and eliminates the possibility for this reaction to create a bottleneck in the breakout from the hot CNO cycle.