58Ni(3He,t)58Cu*(γ) measurements with GODDESS to constrain the astrophysical rate of 57Ni(p,γ)58Cu

S. R. Carmichael; S. D. Pain; M. Siciliano; J. Allen; D. W. Bardayan; C. Boomershine; C. M. Campbell; M. P. Carpenter; K. A. Chipps; J. A. Cizewski; P. A. Copp; J. Forson; H. Garland; R. Ghirmire; J. Kovoor; T. Lauritsen; C. Müller-Gatermann; P. D. O'Malley; A. Ratkiewicz; W. Reviol; D. Seweryniak; H. Sims; C. C. Ummel; G. Wilson

doi:10.1088/1742-6596/2586/1/012109

⁵⁸Ni(³He,t)⁵⁸Cu*(γ) measurements with GODDESS to constrain the astrophysical rate of ⁵⁷Ni(p,γ)⁵⁸Cu

S. R. Carmichael, S. D. Pain, M. Siciliano, J. Allen, D. W. Bardayan, C. Boomershine, C. M. Campbell, M. P. Carpenter, K. A. Chipps, J. A. Cizewski, P. A. Copp, J. Forson, H. Garland, R. Ghirmire, J. Kovoor, T. Lauritsen, C. Müller-Gatermann, P. D. O'Malley, A. Ratkiewicz, W. ReviolD. Seweryniak, H. Sims, C. C. Ummel, G. Wilson

Nuclear Structure and Nuclear Astrophysi

Research output: Contribution to journal › Conference article › peer-review

Abstract

The observation of γ rays from the decay of ⁴⁴Ti in the remnants of core-collapse supernovae (CCSNe) provides crucial information regarding the nucleosynthesis occurring in these events, as ⁴⁴Ti production is sensitive to CCSNe conditions. The final abundance of ⁴⁴Ti is also sensitive to specific nuclear input parameters, one of which is the ⁵⁷Ni(p,γ)⁵⁸Cu reaction rate. A precise rate for ⁵⁷Ni(p,γ)⁵⁸Cu is thus critical if ⁴⁴Ti production is to be an effective probe into CCSNe. To experimentally constrain the ⁵⁷Ni(p,γ)⁵⁸Cu rate, the structure properties of ⁵⁸Cu were measured via the ⁵⁸Ni(³He,t)⁵⁸Cu*(γ) reaction using GODDESS (GRETINA ORRUBA Dual Detectors for Experimental Structure Studies) at Argonne National Laboratory's ATLAS facility. Details of the experiment, ongoing analysis, and plans are presented.

Original language	English
Article number	012109
Journal	Journal of Physics: Conference Series
Volume	2586
Issue number	1
DOIs	https://doi.org/10.1088/1742-6596/2586/1/012109
State	Published - 2023
Event	28th International Nuclear Physics Conference, INPC 2022 - Cape Town, South Africa Duration: Sep 11 2022 → Sep 16 2022

Funding

Research supported by the following institutions: University of Notre Dame (NSF grant no. PHY-2011890), Rutgers University (NSF grant number PHY-1812316 and DOE NNSA contract no. DE-NA0003897), Argonne National Laboratory (DOE Office of Science (NP) contract no. DE-AC02-06CH11357), Oak Ridge National Laboratory (DOE Office of Science (NP) contract no. DE-AC05-00OR22725), Lawrence Livermore National Laboratory (DOE Office of Science (NP) contract no. DE-AC52-07NA27344), University of Tennessee (DOE Office of Science (NP) contract no. DE-FG02-96ER40963). Research supported by the following institutions: University of Notre Dame (NSF grant no. PHY-2011890), Rutgers University (NSF grant number PHY-1812316 and DOE NNSA contract no. DE-NA0003897), Argonne National Laboratory (DOE Office of Science (NP) contract no. DE-AC02-06CH11357), Oak Ridge National Laboratory (DOE Office of Science (NP) contract no. DE-AC05-00OR22725), Lawrence Livermore National Laboratory (DOE Office of Science (NP) contract no. DE-AC52-07NA27344), University of Tennessee (DOE Office of Science (NP) contract no. DE-FG02-96ER40963). This research used resources of Argonne National Laboratory's ATLAS facility, which is a Department of Energy Office of Science User Facility. This material is based upon work supported by the U.S. Department of Energy, Office of Science, Office of Workforce Development for Teachers and Scientists, Office of Science Graduate Student Research (SCGSR) program. The SCGSR program is administered by the Oak Ridge Institute for Science and Education (ORISE) for the DOE. ORISE is managed by ORAU under contract number DE-SC0014664. This research used resources of Argonne National Laboratory’s ATLAS facility, which is a Department of Energy Office of Science User Facility. This material is based upon work supported by the U.S. Department of Energy, Office of Science, Office of Workforce Development for Teachers and Scientists, Office of Science Graduate Student Research (SCGSR) program. The SCGSR program is administered by the Oak Ridge Institute for Science and Education (ORISE) for the DOE. ORISE is managed by ORAU under contract number DE-SC0014664.

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Carmichael, S. R., Pain, S. D., Siciliano, M., Allen, J., Bardayan, D. W., Boomershine, C., Campbell, C. M., Carpenter, M. P., Chipps, K. A., Cizewski, J. A., Copp, P. A., Forson, J., Garland, H., Ghirmire, R., Kovoor, J., Lauritsen, T., Müller-Gatermann, C., O'Malley, P. D., Ratkiewicz, A., ... Wilson, G. (2023). ⁵⁸Ni(³He,t)⁵⁸Cu*(γ) measurements with GODDESS to constrain the astrophysical rate of ⁵⁷Ni(p,γ)⁵⁸Cu. Journal of Physics: Conference Series, 2586(1), Article 012109. https://doi.org/10.1088/1742-6596/2586/1/012109

@article{6e4c8f0cf8a6443c9f668d4cdf18dd9f,

title = "58Ni(3He,t)58Cu*(γ) measurements with GODDESS to constrain the astrophysical rate of 57Ni(p,γ)58Cu",

abstract = "The observation of γ rays from the decay of 44Ti in the remnants of core-collapse supernovae (CCSNe) provides crucial information regarding the nucleosynthesis occurring in these events, as 44Ti production is sensitive to CCSNe conditions. The final abundance of 44Ti is also sensitive to specific nuclear input parameters, one of which is the 57Ni(p,γ)58Cu reaction rate. A precise rate for 57Ni(p,γ)58Cu is thus critical if 44Ti production is to be an effective probe into CCSNe. To experimentally constrain the 57Ni(p,γ)58Cu rate, the structure properties of 58Cu were measured via the 58Ni(3He,t)58Cu*(γ) reaction using GODDESS (GRETINA ORRUBA Dual Detectors for Experimental Structure Studies) at Argonne National Laboratory's ATLAS facility. Details of the experiment, ongoing analysis, and plans are presented.",

author = "Carmichael, \{S. R.\} and Pain, \{S. D.\} and M. Siciliano and J. Allen and Bardayan, \{D. W.\} and C. Boomershine and Campbell, \{C. M.\} and Carpenter, \{M. P.\} and Chipps, \{K. A.\} and Cizewski, \{J. A.\} and Copp, \{P. A.\} and J. Forson and H. Garland and R. Ghirmire and J. Kovoor and T. Lauritsen and C. M{\"u}ller-Gatermann and O'Malley, \{P. D.\} and A. Ratkiewicz and W. Reviol and D. Seweryniak and H. Sims and Ummel, \{C. C.\} and G. Wilson",

note = "Publisher Copyright: {\textcopyright} 2023 Institute of Physics Publishing. All rights reserved.; 28th International Nuclear Physics Conference, INPC 2022 ; Conference date: 11-09-2022 Through 16-09-2022",

year = "2023",

doi = "10.1088/1742-6596/2586/1/012109",

language = "English",

volume = "2586",

journal = "Journal of Physics: Conference Series",

issn = "1742-6588",

number = "1",

}

Carmichael, SR, Pain, SD, Siciliano, M, Allen, J, Bardayan, DW, Boomershine, C, Campbell, CM, Carpenter, MP, Chipps, KA, Cizewski, JA, Copp, PA, Forson, J, Garland, H, Ghirmire, R, Kovoor, J, Lauritsen, T, Müller-Gatermann, C, O'Malley, PD, Ratkiewicz, A, Reviol, W, Seweryniak, D, Sims, H, Ummel, CC & Wilson, G 2023, '⁵⁸Ni(³He,t)⁵⁸Cu*(γ) measurements with GODDESS to constrain the astrophysical rate of ⁵⁷Ni(p,γ)⁵⁸Cu', Journal of Physics: Conference Series, vol. 2586, no. 1, 012109. https://doi.org/10.1088/1742-6596/2586/1/012109

TY - JOUR

T1 - 58Ni(3He,t)58Cu*(γ) measurements with GODDESS to constrain the astrophysical rate of 57Ni(p,γ)58Cu

AU - Carmichael, S. R.

AU - Pain, S. D.

AU - Siciliano, M.

AU - Allen, J.

AU - Bardayan, D. W.

AU - Boomershine, C.

AU - Campbell, C. M.

AU - Carpenter, M. P.

AU - Chipps, K. A.

AU - Cizewski, J. A.

AU - Copp, P. A.

AU - Forson, J.

AU - Garland, H.

AU - Ghirmire, R.

AU - Kovoor, J.

AU - Lauritsen, T.

AU - Müller-Gatermann, C.

AU - O'Malley, P. D.

AU - Ratkiewicz, A.

AU - Reviol, W.

AU - Seweryniak, D.

AU - Sims, H.

AU - Ummel, C. C.

AU - Wilson, G.

PY - 2023

Y1 - 2023

N2 - The observation of γ rays from the decay of 44Ti in the remnants of core-collapse supernovae (CCSNe) provides crucial information regarding the nucleosynthesis occurring in these events, as 44Ti production is sensitive to CCSNe conditions. The final abundance of 44Ti is also sensitive to specific nuclear input parameters, one of which is the 57Ni(p,γ)58Cu reaction rate. A precise rate for 57Ni(p,γ)58Cu is thus critical if 44Ti production is to be an effective probe into CCSNe. To experimentally constrain the 57Ni(p,γ)58Cu rate, the structure properties of 58Cu were measured via the 58Ni(3He,t)58Cu*(γ) reaction using GODDESS (GRETINA ORRUBA Dual Detectors for Experimental Structure Studies) at Argonne National Laboratory's ATLAS facility. Details of the experiment, ongoing analysis, and plans are presented.

AB - The observation of γ rays from the decay of 44Ti in the remnants of core-collapse supernovae (CCSNe) provides crucial information regarding the nucleosynthesis occurring in these events, as 44Ti production is sensitive to CCSNe conditions. The final abundance of 44Ti is also sensitive to specific nuclear input parameters, one of which is the 57Ni(p,γ)58Cu reaction rate. A precise rate for 57Ni(p,γ)58Cu is thus critical if 44Ti production is to be an effective probe into CCSNe. To experimentally constrain the 57Ni(p,γ)58Cu rate, the structure properties of 58Cu were measured via the 58Ni(3He,t)58Cu*(γ) reaction using GODDESS (GRETINA ORRUBA Dual Detectors for Experimental Structure Studies) at Argonne National Laboratory's ATLAS facility. Details of the experiment, ongoing analysis, and plans are presented.

UR - https://www.scopus.com/pages/publications/85174600131

U2 - 10.1088/1742-6596/2586/1/012109

DO - 10.1088/1742-6596/2586/1/012109

M3 - Conference article

AN - SCOPUS:85174600131

SN - 1742-6588

VL - 2586

JO - Journal of Physics: Conference Series

JF - Journal of Physics: Conference Series

IS - 1

M1 - 012109

T2 - 28th International Nuclear Physics Conference, INPC 2022

Y2 - 11 September 2022 through 16 September 2022

ER -

⁵⁸Ni(³He,t)⁵⁸Cu*(γ) measurements with GODDESS to constrain the astrophysical rate of ⁵⁷Ni(p,γ)⁵⁸Cu

Abstract

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