The ORNL Deuterated Spectroscopic Array — ODeSA

Febbraro, M.; Toomey, Rebecca; Pain, S. D.; Chipps, K. A.; Becker, B. R.; Newby, Robert Jason; Meisel, Z.; Massey, T. N.; Brune, C. R.; Liu, Q.; deBoer, R. J.; Macon, K. T.; Boeltzig, A.; O’Neill, J.; Smith, M. S.; Wiescher, M.; Soltesz, D.; Sultana, I.; Brandenburg, K.; Subedi, S. K.; Paneru, S. N.; Danley, T. W.; Alberty-Jones, Y.

doi:10.1016/j.nima.2019.162668

Cited by 8 publications

(5 citation statements)

References 12 publications

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“…The detector response has been calibrated against the well known thick-target spectrum of the 9 Be(d, n) reaction over an energy range that spans those of the present measurements [23]. These calibration measurements were performed at the Edwards Accelerator Laboratory at Ohio University [24]. The detector response was modeled using MCNP-Polimi [25].…”

Section: Fig 2 (Color Online)mentioning

confidence: 99%

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Measurement of the B10(α,n0)13N cross section

et al. 2019

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The National Ignition Facility provides the opportunity to study nuclear reactions under controlled conditions at high temperatures and pressures at a level never before achieved. However, the time scale of the deuterium-tritium (DT) implosion is only a few nanoseconds, making data collection and diagnostics very challenging. One method that has been proposed for obtaining additional information about the conditions of the implosion is to activate a dopant material using the αparticles produced from the DT fuel as a diagnostic. The yield of the activated material can give a measure of the mixing that occurs in the capsule. One of the reactions that has been proposed is 10 B(α, n) 13 N, as it produces a radioactive reactant product with an convenient halflife of ≈10 minutes. While this reaction has several advantages for the application at hand, it has not seen much study in the present literature, resulting in large uncertainties in the cross section. Further, for the current application, the cross section must be well characterized. With this motivation, the 10 B(α, n) 13 N cross section has been remeasured from 2.2 < Eα < 4.9 MeV, with the angle integrated ground state cross section reported for the first time. The present results, combined with previous measurements, allow for a determination of the cross section to a significantly higher degree of accuracy and precision than obtained previously, and are shown to be consistent with thick-target measurements. Preliminary calculations are performed to test the feasibility of this reaction as a diagnostic for a NIF implosion.

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Section: Fig 2 (Color Online)mentioning

confidence: 99%

“…Comparison of the efficiency curve of an 7.6 cm thick × 5.8 cm diameter EJ-315M deuterated liquid scintillator from a simulation using MCNP-Polimi (red triangles) and the efficiency curve measured using time-offlight with the 9 Be(d, n) thick target method [23,24] (blue squares).…”

Section: Fig 3 (Color Online)mentioning

confidence: 99%

Measurement of the B10(α,n0)13N cross section

et al. 2019

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“…Since the intrinsic efficiency of the deuterated liquid scintillators is threshold dependent, neutrons with energies lower than 1 MeV were cut off. The simulation is compared to the experimentally measured efficiency reported by Febbraro et al [59], which was obtained using the 27 Al(d,n) 28 Si reaction at E d = 7.44 MeV and the 9 Be(d,n) 10 B reaction at E d = 7.00 MeV [60,61] at Ohio University. The efficiency is estimated to have an uncertainty of 10%.…”

Section: B Deuterated Liquid Scintillator Detector Efficiencymentioning

confidence: 93%

“…The response matrix is modeled using MCNP-Polomi [57,58] and tuned to match calibration measurements by way of phenomenological descriptions of the light response and resolution functions [59].…”

Section: A Spectrum Unfolding By the Mlem Methodsmentioning

confidence: 99%

Low-energy cross-section measurement of the B10(α,n)N13 reaction and its impact on ne

et al. 2020

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Nucleosynthesis in the first generation of massive stars offers a unique setting to explore the creation of the first heavier nuclei in an environment free of impurities from earlier stellar generations. In later generations of massive stars, hydrogen burning occurs predominantly through the CNO cycles, but without the carbon, nitrogen, and oxygen to catalyze the reaction sequence, first stars would have to rely on the inefficient pp-chains for their energy production. Observations of second and third generation stars show pronounced abundances of carbon and oxygen isotopes, which suggests a rapid conversion of the primordial abundances to heavier elements. While the triplealpha-process primarily facilitates this conversion, there are alternative reaction sequences, such as the 2 H(α, γ) 6 Li(α, γ) 10 B(α, n) 13 N, that may play a significant role. To study such alternate reaction pathways for production of carbon and heavier nuclei, a number of new measurements are needed. In this work, new measurements are reported for the 10 B(α, n) 13 N reaction, extending the cross section down to 575 keV incident α-particle energy. The measurements were made using a state-of-the-art deuterated liquid scintillator and a spectrum unfolding technique. An R-matrix analysis was performed in order to facilitate a comparison of the underlying nuclear structure with the reaction measurements. An unexpected upturn is observed in the low energy S-factor that indicates the presence of a new low energy resonance. A revised reaction rate is determined that takes into account the present data as well as other previous measurements from the literature that were previously neglected.

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“…As a result, the authors have been investigating the use of neutron spectroscopy via spectrum unfolding for various applications, such as to improve material identification [15] and to reduce uncertainty with neutron multiplicity counting. Previous work has performed spectrum unfolding based on a measured response matrix [9]. Although a measured response is preferred, it is cumbersome (in cost, effort, and scheduling) to directly measure the response of the detector for the required number of discrete neutron energies each with the desired counting statistics.…”

Section: Introductionmentioning

confidence: 99%