Constraints on key O17(α,γ)Ne21 resonances and impact on the weak s process

Williams, M.; Laird, A. M.; Choplin, A.; Adsley, P.; Davids, B.; Greife, U.; Hudson, K.; Hutcheon, D.; Lennarz, A.; Ruiz, C.

doi:10.1103/physrevc.105.065805

Constraints on key O 17 (α,γ) Ne 21 resonances and impact on the weak s process

Journal Article · Tue Jun 21 00:00:00 EDT 2022 · Physical Review. C

DOI:https://doi.org/10.1103/physrevc.105.065805· OSTI ID:1979887

^[1]; Laird, A. M. ^[2]; Choplin, A. ^[3]; Adsley, P. ^[4]; Davids, B. ^[5]; ^[6]; ^[7]; Hutcheon, D. ^[8]; Lennarz, A. ^[9]; Ruiz, C. ^[8]

TRIUMF, Vancouver, BC (Canada); University of York (United Kingdom); OSTI
University of York (United Kingdom)
Université Libre de Bruxelles, Brussels (Belgium)
Texas A & M University, College Station, TX (United States)
TRIUMF, Vancouver, BC (Canada); Simon Fraser University, Burnaby, BC (Canada)
Colorado School of Mines, Golden, CO (United States)
Simon Fraser University, Burnaby, BC (Canada); TRIUMF, Vancouver, BC (Canada)
TRIUMF, Vancouver, BC (Canada)
TRIUMF, Vancouver, BC (Canada); McMaster University, Hamilton, ON (Canada)

The efficiency of the slow neutron-capture process in massive stars is strongly influenced by neutron-capture reactions on light elements. At low metallicity, ¹⁶O is an important neutron absorber, but the effectiveness of ¹⁶O as a light-element neutron poison is modified by competition between subsequent ¹⁷O(α,n)²⁰Ne and ¹⁷O(α,γ)²¹Ne reactions. The strengths of key ¹⁷O(α,γ)²¹Ne resonances within the Gamow window for core helium burning in massive stars are not well constrained by experiment. This work presents more precise measurements of resonances in the energy range E_c.m. = 612–1319 keV. We extract resonance strengths of ωγ₆₃₈ = 4.85 ± 0.79 μeV, ωγ₇₂₁ =13.1$$^{+3.2}_{-2.4}$$ μeV, ωγ₈₁₄ = 7.72 ± 0.55 meV, and ωγ₁₃₁₈ = 136 ±13 meV, for resonances at E_c.m. = 638, 721, 814, and 1318 keV, respectively. We also report an upper limit for the 612 keV resonance of ωγ < 140 neV (95% c.l.), which effectively rules out any significant contribution from this resonance to the reaction rate. From this work, a new ¹⁷O(α,γ)²¹Ne thermonuclear reaction rate is calculated and compared to the literature. The effect of present uncertainties in the ¹⁷O(α,γ)²¹Ne reaction rate on weak s-process yields are then explored using postprocessing calculations based on a rotating 20M_⊙ low-metallicity massive star. The resulting ¹⁷O(α,γ)²¹Ne reaction rate is lower with respect to the preexisting literature and found to enhance weak s-process yields in rotating massive star models.

View Accepted Manuscript (DOE)

Research Organization:: Colorado School of Mines, Golden, CO (United States)

Sponsoring Organization:: Fonds dela Recherche Scientifique (FNRS); Science and Technology Facilities Council (STFC); USDOE Office of Science (SC)

Grant/Contract Number:: FG02-93ER40789

OSTI ID:: 1979887

Journal Information:: Physical Review. C, Journal Name: Physical Review. C Journal Issue: 6 Vol. 105; ISSN 2469-9985

Publisher:: American Physical Society (APS)Copyright Statement

Country of Publication:: United States

Language:: English

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