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Title: Shell-model studies of the astrophysical r p -process reactions S 34 ( p , γ ) Cl 35 and Cl 34 g , m ( p , γ ) Ar 35

Abstract

Background: Dust grains condensed in the outflows of presolar classical novae should have been present in the protosolar nebula. Candidates for such presolar nova grains have been found in primitive meteorites and can in principle be identified by their isotopic ratios, but the ratios predicted by state-of-the-art one-dimensional hydrodynamic models are uncertain due to nuclear-physics uncertainties. Purpose: To theoretically calculate the thermonuclear rates and uncertainties of the S 34 ( p , γ ) Cl 35 and Cl 34 g , m ( p , γ ) Ar 35 reactions and investigate their impacts on the predicted 34S/32S isotopic ratio for presolar nova grains. Method: A shell-model approach in a (0 +1 ) ℏ ω model space was used to calculate the properties of resonances in the 34S(p ,γ )35Cl and 34 g,mCl (p ,γ )35Ar reactions and their thermonuclear rates. Uncertainties were estimated using a Monte Carlo method. The implications of these rates and their uncertainties on sulfur isotopic nova yields were investigated using a postprocessing nucleosynthesis code. The rates for transitions from the ground state of 34Cl as well as from the isomeric first excited state of 34Cl were explicitly calculated. Results: At energies in the resonance region near the proton-emission threshold, many negative-parity states appear. Energies, spectroscopic factors, and proton-decay widths are reported. The resulting thermonuclear rates are compared with previous determinations. Conclusions: The shell-model calculations alone are sufficient to constrain the variation of the 34S/32S ratios to within about 30%. Uncertainties associated with other reactions must also be considered, but in general we find that the 34S/32S ratios are not a robust diagnostic to clearly identify presolar grains made from nova ejecta.

Authors:
ORCiD logo [1]; ORCiD logo [2]; ORCiD logo [3];  [2]; ORCiD logo [4];  [5]; ORCiD logo [6];  [7];  [8];  [7]
  1. Univ. of Stellenbosch, Stellenbosch (South Africa); iThemba LABS, Somerset West (South Africa)
  2. Michigan State Univ., East Lansing, MI (United States). National Superconducting Cyclotron Lab., Joint Inst. for Nuclear Astrophysics–Center for the Evolution of the Elements
  3. North Carolina State Univ., Raleigh, NC (United States); Duke Univ., Durham, NC (United States). Triangle Universities Nuclear Laboratory
  4. Univ. of Victoria, BC (Canada)
  5. Michigan State Univ., East Lansing, MI (United States). National Superconducting Cyclotron Lab.
  6. Univ. of Victoria, BC (Canada); Michigan State Univ., East Lansing, MI (United States). Joint Inst. for Nuclear Astrophysics–Center for the Evolution of the Elements
  7. Goethe Univ., Frankfurt (Germany)
  8. Univ. of Hull, Hull (United Kingdom). E.A. Milne Center for Astrophysics; Hungarian Academy of Sciences, Budapest (Hungary). Konkoly Observatory, Research Center for Astronomy and Earth Sciences; Michigan State Univ., East Lansing, MI (United States). Joint Inst. for Nuclear Astrophysics–Center for the Evolution of the Elements
Publication Date:
Research Org.:
North Carolina State University, Raleigh, NC (United States)
Sponsoring Org.:
USDOE Office of Science (SC), Nuclear Physics (NP); Hungarian Academy of Sciences (Hungary); National Science Foundation (NSF); University of Stellenbosch (South Africa); iThemba LABS (South Africa); University of Hull
OSTI Identifier:
1774782
Grant/Contract Number:  
SC0017799; SC0016052; FG02-97ER41041; PHY-1811855; PHY-1565546; PHY-1913554; PHY-1430152; ST/R000840/1
Resource Type:
Accepted Manuscript
Journal Name:
Physical Review C
Additional Journal Information:
Journal Volume: 102; Journal Issue: 2; Journal ID: ISSN 2469-9985
Publisher:
American Physical Society (APS)
Country of Publication:
United States
Language:
English
Subject:
73 NUCLEAR PHYSICS AND RADIATION PHYSICS

Citation Formats

Richter, W. A., Brown, B. A., Longland, R., Wrede, C., Denissenkov, P., Fry, C., Herwig, F., Kurtulgil, D., Pignatari, M., and Reifarth, R. Shell-model studies of the astrophysical r p -process reactions S 34 ( p , γ ) Cl 35 and Cl 34 g , m ( p , γ ) Ar 35. United States: N. p., 2020. Web. doi:10.1103/physrevc.102.025801.
Richter, W. A., Brown, B. A., Longland, R., Wrede, C., Denissenkov, P., Fry, C., Herwig, F., Kurtulgil, D., Pignatari, M., & Reifarth, R. Shell-model studies of the astrophysical r p -process reactions S 34 ( p , γ ) Cl 35 and Cl 34 g , m ( p , γ ) Ar 35. United States. https://doi.org/10.1103/physrevc.102.025801
Richter, W. A., Brown, B. A., Longland, R., Wrede, C., Denissenkov, P., Fry, C., Herwig, F., Kurtulgil, D., Pignatari, M., and Reifarth, R. Tue . "Shell-model studies of the astrophysical r p -process reactions S 34 ( p , γ ) Cl 35 and Cl 34 g , m ( p , γ ) Ar 35". United States. https://doi.org/10.1103/physrevc.102.025801. https://www.osti.gov/servlets/purl/1774782.
@article{osti_1774782,
title = {Shell-model studies of the astrophysical r p -process reactions S 34 ( p , γ ) Cl 35 and Cl 34 g , m ( p , γ ) Ar 35},
author = {Richter, W. A. and Brown, B. A. and Longland, R. and Wrede, C. and Denissenkov, P. and Fry, C. and Herwig, F. and Kurtulgil, D. and Pignatari, M. and Reifarth, R.},
abstractNote = {Background: Dust grains condensed in the outflows of presolar classical novae should have been present in the protosolar nebula. Candidates for such presolar nova grains have been found in primitive meteorites and can in principle be identified by their isotopic ratios, but the ratios predicted by state-of-the-art one-dimensional hydrodynamic models are uncertain due to nuclear-physics uncertainties. Purpose: To theoretically calculate the thermonuclear rates and uncertainties of the S 34 ( p , γ ) Cl 35 and Cl 34 g , m ( p , γ ) Ar 35 reactions and investigate their impacts on the predicted 34S/32S isotopic ratio for presolar nova grains. Method: A shell-model approach in a (0 +1 ) ℏ ω model space was used to calculate the properties of resonances in the 34S(p ,γ )35Cl and 34 g,mCl (p ,γ )35Ar reactions and their thermonuclear rates. Uncertainties were estimated using a Monte Carlo method. The implications of these rates and their uncertainties on sulfur isotopic nova yields were investigated using a postprocessing nucleosynthesis code. The rates for transitions from the ground state of 34Cl as well as from the isomeric first excited state of 34Cl were explicitly calculated. Results: At energies in the resonance region near the proton-emission threshold, many negative-parity states appear. Energies, spectroscopic factors, and proton-decay widths are reported. The resulting thermonuclear rates are compared with previous determinations. Conclusions: The shell-model calculations alone are sufficient to constrain the variation of the 34S/32S ratios to within about 30%. Uncertainties associated with other reactions must also be considered, but in general we find that the 34S/32S ratios are not a robust diagnostic to clearly identify presolar grains made from nova ejecta.},
doi = {10.1103/physrevc.102.025801},
journal = {Physical Review C},
number = 2,
volume = 102,
place = {United States},
year = {Tue Aug 04 00:00:00 EDT 2020},
month = {Tue Aug 04 00:00:00 EDT 2020}
}

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