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Title: A direct measurement of the 17O(α,γ)21Ne reaction in inverse kinematics and its impact on heavy element production

Abstract

During the slow neutron capture process in massive stars, reactions on light elements can both produce and absorb neutrons thereby influencing the final heavy element abundances. At low metallicities, the high neutron capture rate of 16O can inhibit s-process nucleosynthesis unless the neutrons are recycled via the 17O(α, n)20Ne reaction. The efficiency of this neutron recycling is determined by competition between the 17O(α, n)20Ne and 17O(α, γ)21Ne reactions. While some experimental data are available on the former reaction, no data exist for the radiative capture channel at the relevant astrophysical energies. The 17O(α, γ)21Ne reaction has been studied directly using the DRAGON recoil separator at the TRIUMF Laboratory. The reaction cross section has been determined at energies between 0.6 and 1.6 MeV Ecm, reaching into the Gamow window for core helium burning for the first time. Resonance strengths for resonances at 0.63, 0.721, 0.81 and 1.122 MeV Ecmhave been extracted. The experimentally based reaction rate calculated represents a lower limit, but suggests that significant s-process nucleosynthesis occurs in low metallicity massive stars.

Authors:
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Publication Date:
Research Org.:
Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States)
Sponsoring Org.:
USDOE; National Science Foundation (NSF)
Contributing Org.:
NuGrid Collaboration
OSTI Identifier:
1559356
Alternate Identifier(s):
OSTI ID: 1566949
Grant/Contract Number:  
FG02-93ER40789; AC05-00OR22725
Resource Type:
Published Article
Journal Name:
Physics Letters B
Additional Journal Information:
Journal Name: Physics Letters B Journal Volume: 798 Journal Issue: C; Journal ID: ISSN 0370-2693
Publisher:
Elsevier
Country of Publication:
Netherlands
Language:
English
Subject:
74 ATOMIC AND MOLECULAR PHYSICS

Citation Formats

Taggart, M. P., Akers, C., Laird, A. M., Hager, U., Ruiz, C., Hutcheon, D. A., Bentley, M. A., Brown, J. R., Buchmann, L., Chen, A. A., Chen, J., Chipps, K. A., Choplin, A., D'Auria, J. M., Davids, B., Davis, C., Diget, C. Aa., Erikson, L., Fallis, J., Fox, S. P., Frischknecht, U., Fulton, B. R., Galinski, N., Greife, U., Hirschi, R., Howell, D., Martin, L., Mountford, D., Murphy, A. St. J., Ottewell, D., Pignatari, M., Reeve, S., Ruprecht, G., Sjue, S., Veloce, L., and Williams, M.. A direct measurement of the 17O(α,γ)21Ne reaction in inverse kinematics and its impact on heavy element production. Netherlands: N. p., 2019. Web. https://doi.org/10.1016/j.physletb.2019.134894.
Taggart, M. P., Akers, C., Laird, A. M., Hager, U., Ruiz, C., Hutcheon, D. A., Bentley, M. A., Brown, J. R., Buchmann, L., Chen, A. A., Chen, J., Chipps, K. A., Choplin, A., D'Auria, J. M., Davids, B., Davis, C., Diget, C. Aa., Erikson, L., Fallis, J., Fox, S. P., Frischknecht, U., Fulton, B. R., Galinski, N., Greife, U., Hirschi, R., Howell, D., Martin, L., Mountford, D., Murphy, A. St. J., Ottewell, D., Pignatari, M., Reeve, S., Ruprecht, G., Sjue, S., Veloce, L., & Williams, M.. A direct measurement of the 17O(α,γ)21Ne reaction in inverse kinematics and its impact on heavy element production. Netherlands. https://doi.org/10.1016/j.physletb.2019.134894
Taggart, M. P., Akers, C., Laird, A. M., Hager, U., Ruiz, C., Hutcheon, D. A., Bentley, M. A., Brown, J. R., Buchmann, L., Chen, A. A., Chen, J., Chipps, K. A., Choplin, A., D'Auria, J. M., Davids, B., Davis, C., Diget, C. Aa., Erikson, L., Fallis, J., Fox, S. P., Frischknecht, U., Fulton, B. R., Galinski, N., Greife, U., Hirschi, R., Howell, D., Martin, L., Mountford, D., Murphy, A. St. J., Ottewell, D., Pignatari, M., Reeve, S., Ruprecht, G., Sjue, S., Veloce, L., and Williams, M.. Fri . "A direct measurement of the 17O(α,γ)21Ne reaction in inverse kinematics and its impact on heavy element production". Netherlands. https://doi.org/10.1016/j.physletb.2019.134894.
@article{osti_1559356,
title = {A direct measurement of the 17O(α,γ)21Ne reaction in inverse kinematics and its impact on heavy element production},
author = {Taggart, M. P. and Akers, C. and Laird, A. M. and Hager, U. and Ruiz, C. and Hutcheon, D. A. and Bentley, M. A. and Brown, J. R. and Buchmann, L. and Chen, A. A. and Chen, J. and Chipps, K. A. and Choplin, A. and D'Auria, J. M. and Davids, B. and Davis, C. and Diget, C. Aa. and Erikson, L. and Fallis, J. and Fox, S. P. and Frischknecht, U. and Fulton, B. R. and Galinski, N. and Greife, U. and Hirschi, R. and Howell, D. and Martin, L. and Mountford, D. and Murphy, A. St. J. and Ottewell, D. and Pignatari, M. and Reeve, S. and Ruprecht, G. and Sjue, S. and Veloce, L. and Williams, M.},
abstractNote = {During the slow neutron capture process in massive stars, reactions on light elements can both produce and absorb neutrons thereby influencing the final heavy element abundances. At low metallicities, the high neutron capture rate of 16O can inhibit s-process nucleosynthesis unless the neutrons are recycled via the 17O(α, n)20Ne reaction. The efficiency of this neutron recycling is determined by competition between the 17O(α, n)20Ne and 17O(α, γ)21Ne reactions. While some experimental data are available on the former reaction, no data exist for the radiative capture channel at the relevant astrophysical energies. The 17O(α, γ)21Ne reaction has been studied directly using the DRAGON recoil separator at the TRIUMF Laboratory. The reaction cross section has been determined at energies between 0.6 and 1.6 MeV Ecm, reaching into the Gamow window for core helium burning for the first time. Resonance strengths for resonances at 0.63, 0.721, 0.81 and 1.122 MeV Ecmhave been extracted. The experimentally based reaction rate calculated represents a lower limit, but suggests that significant s-process nucleosynthesis occurs in low metallicity massive stars.},
doi = {10.1016/j.physletb.2019.134894},
journal = {Physics Letters B},
number = C,
volume = 798,
place = {Netherlands},
year = {2019},
month = {11}
}

Journal Article:
Free Publicly Available Full Text
Publisher's Version of Record
https://doi.org/10.1016/j.physletb.2019.134894

Figures / Tables:

Fig. 1 Fig. 1: Part of 21Ne level scheme. The Gamow window for the 17O($α, γ$ )21Ne reaction during core helium burning in massive stars is indicated by the bar on the left and the bars on the right show the energy regions covered by the present work.

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Figures/Tables have been extracted from DOE-funded journal article accepted manuscripts.