Resonant scattering of 22Na + p studied by the thick-target inverse-kinematic method

S. J. Jin, Y. B. Wang, J. Su, S. Q. Yan, Y. J. Li, B. Guo, Z. H. Li, S. Zeng, G. Lian, X. X. Bai, W. P. Liu, H. Yamaguchi, S. Kubono, J. Hu, D. Kahl, H. S. Jung, J. Y. Moon, C. S. Lee, Takashi Teranishi, H. W. Wang & 4 others H. Ishiyama, N. Iwasa, T. Komatsubara, B. A. Brown

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Abstract

Background: In presolar low-density graphite grains, an extraordinarily large 22Ne/20Ne ratio or even nearly pure 22Ne is found, pointing to the condensation of radioactive 22Na in grains. Supernovae and neon-rich novae are the main events that produce 22Na via the explosive hydrogen burning process. The 22Na(p, γ)23Mg reaction is one of the key reactions that influences the 22Na abundance in ejecta. Purpose:The present work aims to explore the proton resonant states in 23Mg relevant to the astrophysical 22Na(p, γ)23Mg reaction. The determined 23Mg resonant parameters can be used to evaluate the 22Na(p, γ)23Mg reaction rate. Method:A low-energy 22Na radioactive ion beam is produced via the 1H(22Ne, 22Na)n reaction, and used to measure the experimental excitation function of the 22Na + p resonant scattering with a conventional thick-target inverse kinematic method. R-matrix analysis is applied to deduce the 23Mg resonance parameters from the experimental excitation function. Results: Three proton resonance states in 23Mg are observed. Spins/parities and the proton partial widths are determined. The deduced excitation energies agree with the compiled values. Conclusions: The new spin and parity assignments allow us to perform a shell-model calculation of the γ widths of the 23Mg resonant states for the evaluation of the 22Na(p, γ)23Mg astrophysical reaction rate. The two s-wave resonant states established in this work at 8.793 and 8.916 MeV in 23Mg, respectively, increase the total reaction rate by about 5% at a temperature greater than 2 GK.

Original languageEnglish
Article number035801
JournalPhysical Review C - Nuclear Physics
Volume88
Issue number3
DOIs
Publication statusPublished - Sep 3 2013

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inverse kinematics
reaction kinetics
scattering
astrophysics
parity
excitation
proton resonance
novae
protons
ejecta
neon
supernovae
graphite
condensation
ion beams
energy
evaluation
hydrogen
temperature

All Science Journal Classification (ASJC) codes

  • Nuclear and High Energy Physics

Cite this

Jin, S. J., Wang, Y. B., Su, J., Yan, S. Q., Li, Y. J., Guo, B., ... Brown, B. A. (2013). Resonant scattering of 22Na + p studied by the thick-target inverse-kinematic method. Physical Review C - Nuclear Physics, 88(3), [035801]. https://doi.org/10.1103/PhysRevC.88.035801

Resonant scattering of 22Na + p studied by the thick-target inverse-kinematic method. / Jin, S. J.; Wang, Y. B.; Su, J.; Yan, S. Q.; Li, Y. J.; Guo, B.; Li, Z. H.; Zeng, S.; Lian, G.; Bai, X. X.; Liu, W. P.; Yamaguchi, H.; Kubono, S.; Hu, J.; Kahl, D.; Jung, H. S.; Moon, J. Y.; Lee, C. S.; Teranishi, Takashi; Wang, H. W.; Ishiyama, H.; Iwasa, N.; Komatsubara, T.; Brown, B. A.

In: Physical Review C - Nuclear Physics, Vol. 88, No. 3, 035801, 03.09.2013.

Research output: Contribution to journalArticle

Jin, SJ, Wang, YB, Su, J, Yan, SQ, Li, YJ, Guo, B, Li, ZH, Zeng, S, Lian, G, Bai, XX, Liu, WP, Yamaguchi, H, Kubono, S, Hu, J, Kahl, D, Jung, HS, Moon, JY, Lee, CS, Teranishi, T, Wang, HW, Ishiyama, H, Iwasa, N, Komatsubara, T & Brown, BA 2013, 'Resonant scattering of 22Na + p studied by the thick-target inverse-kinematic method', Physical Review C - Nuclear Physics, vol. 88, no. 3, 035801. https://doi.org/10.1103/PhysRevC.88.035801
Jin, S. J. ; Wang, Y. B. ; Su, J. ; Yan, S. Q. ; Li, Y. J. ; Guo, B. ; Li, Z. H. ; Zeng, S. ; Lian, G. ; Bai, X. X. ; Liu, W. P. ; Yamaguchi, H. ; Kubono, S. ; Hu, J. ; Kahl, D. ; Jung, H. S. ; Moon, J. Y. ; Lee, C. S. ; Teranishi, Takashi ; Wang, H. W. ; Ishiyama, H. ; Iwasa, N. ; Komatsubara, T. ; Brown, B. A. / Resonant scattering of 22Na + p studied by the thick-target inverse-kinematic method. In: Physical Review C - Nuclear Physics. 2013 ; Vol. 88, No. 3.
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abstract = "Background: In presolar low-density graphite grains, an extraordinarily large 22Ne/20Ne ratio or even nearly pure 22Ne is found, pointing to the condensation of radioactive 22Na in grains. Supernovae and neon-rich novae are the main events that produce 22Na via the explosive hydrogen burning process. The 22Na(p, γ)23Mg reaction is one of the key reactions that influences the 22Na abundance in ejecta. Purpose:The present work aims to explore the proton resonant states in 23Mg relevant to the astrophysical 22Na(p, γ)23Mg reaction. The determined 23Mg resonant parameters can be used to evaluate the 22Na(p, γ)23Mg reaction rate. Method:A low-energy 22Na radioactive ion beam is produced via the 1H(22Ne, 22Na)n reaction, and used to measure the experimental excitation function of the 22Na + p resonant scattering with a conventional thick-target inverse kinematic method. R-matrix analysis is applied to deduce the 23Mg resonance parameters from the experimental excitation function. Results: Three proton resonance states in 23Mg are observed. Spins/parities and the proton partial widths are determined. The deduced excitation energies agree with the compiled values. Conclusions: The new spin and parity assignments allow us to perform a shell-model calculation of the γ widths of the 23Mg resonant states for the evaluation of the 22Na(p, γ)23Mg astrophysical reaction rate. The two s-wave resonant states established in this work at 8.793 and 8.916 MeV in 23Mg, respectively, increase the total reaction rate by about 5{\%} at a temperature greater than 2 GK.",
author = "Jin, {S. J.} and Wang, {Y. B.} and J. Su and Yan, {S. Q.} and Li, {Y. J.} and B. Guo and Li, {Z. H.} and S. Zeng and G. Lian and Bai, {X. X.} and Liu, {W. P.} and H. Yamaguchi and S. Kubono and J. Hu and D. Kahl and Jung, {H. S.} and Moon, {J. Y.} and Lee, {C. S.} and Takashi Teranishi and Wang, {H. W.} and H. Ishiyama and N. Iwasa and T. Komatsubara and Brown, {B. A.}",
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T1 - Resonant scattering of 22Na + p studied by the thick-target inverse-kinematic method

AU - Jin, S. J.

AU - Wang, Y. B.

AU - Su, J.

AU - Yan, S. Q.

AU - Li, Y. J.

AU - Guo, B.

AU - Li, Z. H.

AU - Zeng, S.

AU - Lian, G.

AU - Bai, X. X.

AU - Liu, W. P.

AU - Yamaguchi, H.

AU - Kubono, S.

AU - Hu, J.

AU - Kahl, D.

AU - Jung, H. S.

AU - Moon, J. Y.

AU - Lee, C. S.

AU - Teranishi, Takashi

AU - Wang, H. W.

AU - Ishiyama, H.

AU - Iwasa, N.

AU - Komatsubara, T.

AU - Brown, B. A.

PY - 2013/9/3

Y1 - 2013/9/3

N2 - Background: In presolar low-density graphite grains, an extraordinarily large 22Ne/20Ne ratio or even nearly pure 22Ne is found, pointing to the condensation of radioactive 22Na in grains. Supernovae and neon-rich novae are the main events that produce 22Na via the explosive hydrogen burning process. The 22Na(p, γ)23Mg reaction is one of the key reactions that influences the 22Na abundance in ejecta. Purpose:The present work aims to explore the proton resonant states in 23Mg relevant to the astrophysical 22Na(p, γ)23Mg reaction. The determined 23Mg resonant parameters can be used to evaluate the 22Na(p, γ)23Mg reaction rate. Method:A low-energy 22Na radioactive ion beam is produced via the 1H(22Ne, 22Na)n reaction, and used to measure the experimental excitation function of the 22Na + p resonant scattering with a conventional thick-target inverse kinematic method. R-matrix analysis is applied to deduce the 23Mg resonance parameters from the experimental excitation function. Results: Three proton resonance states in 23Mg are observed. Spins/parities and the proton partial widths are determined. The deduced excitation energies agree with the compiled values. Conclusions: The new spin and parity assignments allow us to perform a shell-model calculation of the γ widths of the 23Mg resonant states for the evaluation of the 22Na(p, γ)23Mg astrophysical reaction rate. The two s-wave resonant states established in this work at 8.793 and 8.916 MeV in 23Mg, respectively, increase the total reaction rate by about 5% at a temperature greater than 2 GK.

AB - Background: In presolar low-density graphite grains, an extraordinarily large 22Ne/20Ne ratio or even nearly pure 22Ne is found, pointing to the condensation of radioactive 22Na in grains. Supernovae and neon-rich novae are the main events that produce 22Na via the explosive hydrogen burning process. The 22Na(p, γ)23Mg reaction is one of the key reactions that influences the 22Na abundance in ejecta. Purpose:The present work aims to explore the proton resonant states in 23Mg relevant to the astrophysical 22Na(p, γ)23Mg reaction. The determined 23Mg resonant parameters can be used to evaluate the 22Na(p, γ)23Mg reaction rate. Method:A low-energy 22Na radioactive ion beam is produced via the 1H(22Ne, 22Na)n reaction, and used to measure the experimental excitation function of the 22Na + p resonant scattering with a conventional thick-target inverse kinematic method. R-matrix analysis is applied to deduce the 23Mg resonance parameters from the experimental excitation function. Results: Three proton resonance states in 23Mg are observed. Spins/parities and the proton partial widths are determined. The deduced excitation energies agree with the compiled values. Conclusions: The new spin and parity assignments allow us to perform a shell-model calculation of the γ widths of the 23Mg resonant states for the evaluation of the 22Na(p, γ)23Mg astrophysical reaction rate. The two s-wave resonant states established in this work at 8.793 and 8.916 MeV in 23Mg, respectively, increase the total reaction rate by about 5% at a temperature greater than 2 GK.

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