Developing the S32(p,d)S*31(p)(γ) reaction to probe the P30(p,γ)S31 reaction rate in classical novae

Burcher, Sean; Chipps, Kelly A.; Hughes, R. O.; Reingold, C. S.; Saastamoinen, A.; Harke, Jason T.; Cooper, N.; Ahn, S.; Allmond, James Mitchell; Clark, H.; Cizewski, Jolie A.; Hall, Matt R.; Hooker, J.; Jayatissa, Heshani; Jones, Kate L.; Ota, Shuya; Pain, Steven D.; Schmidt, K.; Simon, Anna; Upadhyayula, Sriteja

doi:10.1103/physrevc.105.045805

Title: Developing the S 32 ( p , d ) S * 31 ( p ) ( γ ) reaction to probe the P 30 ( p , γ ) S 31 reaction rate in classical novae

Abstract

Background: The ³⁰P(p,γ)³¹S reaction rate is one of the largest remaining sources of uncertainty in the final abundances of nuclei created in a classical nova involving a ONe white dwarf. The reaction rate directly influences silicon isotopic ratios, which are used as identifiers of presolar grains with nova origins. Additionally, the uncertainty in the ³⁰P(p,γ)³¹S reaction rate has been found to limit the use of nova nuclear thermometers based on observations of elemental ratios in nova ejecta. Purpose: Reduce uncertainties in the nuclear data for proton-unbound states in ³¹S, which act as resonances for the ³⁰P(p,γ)³¹S reaction at classical nova temperatures, and develop a technique for high efficiency, high-resolution reaction-decay coincidence measurements. Methods: Here, the ³²S(p,d)³¹S reaction was used to populate the states of interest in ³¹S. The experiment was performed at the Texas A&M Cyclotron Institute using the LLNL Hyperion array for the detection of charged particles and γ rays. A downstream silicon telescope was used to select reaction deuterons, and a single upstream silicon detector was used to measure protons emitted in the decay of unbound ³¹S levels. Results: Several states in ³¹S above the proton separation energy were observed to have been populated. Decay protons from themore »« less

Authors:

^[1];

^[2]; Hughes, R. O. ^[3]; Reingold, C. S. ^[4]; Saastamoinen, A. ^[5];

^[3]; Cooper, N. ^[6]; Ahn, S. ^[5];

^[7]; Clark, H. ^[5];

^[8]; Hall, Matt R. ^[7]; Hooker, J. ^[5];

^[5];

^[9];

^[5]; Pain, Steven D. ^[7]; Schmidt, K. ^[10];

^[6];

^[5]

Univ. of Tennessee, Knoxville, TN (United States); Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
Univ. of Tennessee, Knoxville, TN (United States); Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States)
Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
Univ. of Notre Dame, IN (United States); Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
Texas A & M Univ., College Station, TX (United States)
Univ. of Notre Dame, IN (United States)
Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States)
Rutgers Univ., New Brunswick, NJ (United States)
Univ. of Tennessee, Knoxville, TN (United States)
Michigan State Univ., East Lansing, MI (United States); Joint Inst. for Nuclear Astrophysics (JINA), East Lansing, MI (United States); Helmholtz-Zentrum Dresden-Rossendorf, Dresden (Germany)

Publication Date:: Fri Apr 22 00:00:00 EDT 2022

Research Org.:: Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States); Lawrence Livermore National Laboratory (LLNL), Livermore, CA (United States)

Sponsoring Org.:: USDOE Office of Science (SC), Nuclear Physics (NP); National Science Foundation (NSF); USDOE Laboratory Directed Research and Development (LDRD) Program; USDOE National Nuclear Security Administration (NNSA)

OSTI Identifier:: 1866696

Alternate Identifier(s):: OSTI ID: 1871854; OSTI ID: 1872298

Report Number(s):: LLNL-JRNL-836142
Journal ID: ISSN 2469-9985; TRN: US2306090

Grant/Contract Number:: AC05-00OR22725; FG02-96ER40983; NA0003780; NA0002132; NA0003841; FG03-93ER40773; AC52-07NA27344; PHY-1430152; PHY-1812316; FG02-96ER40983 (UTK); AC05-00OR22725 (ORNL); NA-0003780 (Notre Dame); NA0002132 (Rutgers); FG03-93ER40773 (TAMU); NA-0003841 (CENTAUR)

Resource Type:: Accepted Manuscript

Journal Name:: Physical Review. C

Additional Journal Information:: Journal Volume: 105; Journal Issue: 4; Journal ID: ISSN 2469-9985

Publisher:: American Physical Society (APS)

Country of Publication:: United States

Language:: English

Subject:: 73 NUCLEAR PHYSICS AND RADIATION PHYSICS; explosive burning; transient and explosive astronomical phenomena; nucleosynthesis in explosive environments; nuclear astrophysics; nucleon induced nuclear reactions; nuclear reactions; proton emission; nuclear structure and decays; radiative capture; nuclear mass ranges

Citation Formats


                    Burcher, Sean, Chipps, Kelly A., Hughes, R. O., Reingold, C. S., Saastamoinen, A., Harke, Jason T., Cooper, N., Ahn, S., Allmond, James Mitchell, Clark, H., Cizewski, Jolie A., Hall, Matt R., Hooker, J., Jayatissa, Heshani, Jones, Kate L., Ota, Shuya, Pain, Steven D., Schmidt, K., Simon, Anna, and Upadhyayula, Sriteja. Developing the S32(p,d)S*31(p)(γ) reaction to probe the P30(p,γ)S31 reaction rate in classical novae.  United States: N. p., 2022. 
Web.  doi:10.1103/physrevc.105.045805.

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                    Burcher, Sean, Chipps, Kelly A., Hughes, R. O., Reingold, C. S., Saastamoinen, A., Harke, Jason T., Cooper, N., Ahn, S., Allmond, James Mitchell, Clark, H., Cizewski, Jolie A., Hall, Matt R., Hooker, J., Jayatissa, Heshani, Jones, Kate L., Ota, Shuya, Pain, Steven D., Schmidt, K., Simon, Anna, & Upadhyayula, Sriteja. Developing the S32(p,d)S*31(p)(γ) reaction to probe the P30(p,γ)S31 reaction rate in classical novae.  United States.  https://doi.org/10.1103/physrevc.105.045805

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                    Burcher, Sean, Chipps, Kelly A., Hughes, R. O., Reingold, C. S., Saastamoinen, A., Harke, Jason T., Cooper, N., Ahn, S., Allmond, James Mitchell, Clark, H., Cizewski, Jolie A., Hall, Matt R., Hooker, J., Jayatissa, Heshani, Jones, Kate L., Ota, Shuya, Pain, Steven D., Schmidt, K., Simon, Anna, and Upadhyayula, Sriteja. Fri .  
"Developing the S32(p,d)S*31(p)(γ) reaction to probe the P30(p,γ)S31 reaction rate in classical novae".  United States.  https://doi.org/10.1103/physrevc.105.045805.  https://www.osti.gov/servlets/purl/1866696.

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@article{osti_1866696,

  title        = {Developing the S32(p,d)S*31(p)(γ) reaction to probe the P30(p,γ)S31 reaction rate in classical novae},

  author       = {Burcher, Sean and Chipps, Kelly A. and Hughes, R. O. and Reingold, C. S. and Saastamoinen, A. and Harke, Jason T. and Cooper, N. and Ahn, S. and Allmond, James Mitchell and Clark, H. and Cizewski, Jolie A. and Hall, Matt R. and Hooker, J. and Jayatissa, Heshani and Jones, Kate L. and Ota, Shuya and Pain, Steven D. and Schmidt, K. and Simon, Anna and Upadhyayula, Sriteja},

  abstractNote = {Background: The 30P(p,γ)31S reaction rate is one of the largest remaining sources of uncertainty in the final abundances of nuclei created in a classical nova involving a ONe white dwarf. The reaction rate directly influences silicon isotopic ratios, which are used as identifiers of presolar grains with nova origins. Additionally, the uncertainty in the 30P(p,γ)31S reaction rate has been found to limit the use of nova nuclear thermometers based on observations of elemental ratios in nova ejecta. Purpose: Reduce uncertainties in the nuclear data for proton-unbound states in 31S, which act as resonances for the 30P(p,γ)31S reaction at classical nova temperatures, and develop a technique for high efficiency, high-resolution reaction-decay coincidence measurements. Methods: Here, the 32S(p,d)31S reaction was used to populate the states of interest in 31S. The experiment was performed at the Texas A&M Cyclotron Institute using the LLNL Hyperion array for the detection of charged particles and γ rays. A downstream silicon telescope was used to select reaction deuterons, and a single upstream silicon detector was used to measure protons emitted in the decay of unbound 31S levels. Results: Several states in 31S above the proton separation energy were observed to have been populated. Decay protons from the resonant states in 31S were identified as events in the upstream silicon detectors that came in coincidence with deuterons in the downstream telescope. Protons emitted from these states were measured and branching ratios extracted. Conclusions: While no new reaction rate is derived, spin-parity assignments for several higher-lying proton unbound states have been confirmed. Measured p0 branching ratios for these levels have been compared to previous measurements with good agreement, and in some cases provided a reduction in uncertainty. The previously identified T = 3/2 state may have been incorrectly assigned a large p0 branching ratio in a previous measurement. The technique of measuring reaction-decay coincidences with a particle-gamma setup appears promising.},

  doi          = {10.1103/physrevc.105.045805},

  journal      = {Physical Review. C},

  number       = 4,

  volume       = 105,

  place        = {United States},

  year         = {Fri Apr 22 00:00:00 EDT 2022},

  month        = {Fri Apr 22 00:00:00 EDT 2022}

}

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Title: Developing the S 32 ( p , d ) S * 31 ( p ) ( γ ) reaction to probe the P 30 ( p , γ ) S 31 reaction rate in classical novae

Abstract

Citation Formats

Isobaric multiplet mass equation in the A = 31 , T = 3 / 2 quartets journal, June 2016

Detailed study of the decay Cl 31 ( β γ ) S 31 journal, June 2018

Isospin Mixing Reveals P 30 ( p , γ ) S 31 Resonance Influencing Nova Nucleosynthesis journal, March 2016

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Constraint of the Astrophysical ${}^{26 g}{Al} (p, γ) {}^{27}{Si}$ Destruction Rate at Stellar Temperatures
journal, May 2015

Nuclear Mixing Meters for Classical Novae
journal, October 2013

Synthesis of Intermediate‐Mass Elements in Classical Novae: From Si to Ca
journal, October 2001

The Effects of Thermonuclear Reaction‐Rate Variations on Nova Nucleosynthesis: A Sensitivity Study
journal, September 2002

( $p, d$ ) Reaction on $N = Z$ Nuclei in the $2 s - 1 d$ Shell
journal, August 1968

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journal, April 2001

Nuclear Thermometers for Classical Novae
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Astrophysically important ${}^{31}S$ states studied with the ${}^{32}S$ ( $p, d$ ) ${}^{31}S$ reaction
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