抄録
Background: Type I x-ray bursts are the most frequently observed thermonuclear explosions in the galaxy, resulting from thermonuclear runaway on the surface of an accreting neutron star. The S30(α,p) reaction plays a critical role in burst models, yet insufficient experimental information is available to calculate a reliable, precise rate for this reaction. Purpose: Our measurement was conducted to search for states in Ar34 and determine their quantum properties. In particular, natural-parity states with large α-decay partial widths should dominate the stellar reaction rate. Method: We performed the first measurement of S30+α resonant elastic scattering up to a center-of-mass energy of 5.5 MeV using a radioactive ion beam. The experiment utilized a thick gaseous active target system and silicon detector array in inverse kinematics. Results: We obtained an excitation function for S30(α,α) near 150 in the center-of-mass frame. The experimental data were analyzed with R-matrix calculations, and we observed three new resonant patterns between 11.1 and 12.1 MeV, extracting their properties of resonance energy, widths, spin, and parity. Conclusions: We calculated the resonant thermonuclear reaction rate of S30(α,p) based on all available experimental data of Ar34 and found an upper limit about one order of magnitude larger than a rate determined using a statistical model. The astrophysical impact of these two rates has been investigated through one-zone postprocessing type I x-ray burst calculations. We find that our new upper limit for the S30(α,p)Cl33 rate significantly affects the predicted nuclear energy generation rate during the burst.
| 元の言語 | 英語 |
|---|---|
| 記事番号 | 015802 |
| ジャーナル | Physical Review C |
| 巻 | 97 |
| 発行部数 | 1 |
| DOI | |
| 出版物ステータス | 出版済み - 1 3 2018 |
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All Science Journal Classification (ASJC) codes
- Nuclear and High Energy Physics
これを引用
First measurement of S 30 +α resonant elastic scattering for the S 30 (α,p) reaction rate. / Kahl, Daid; Yamaguchi, H.; Kubono, S.; Chen, A. A.; Parikh, A.; Binh, D. N.; Chen, J.; Cherubini, S.; Duy, N. N.; Hashimoto, T.; Hayakawa, S.; Iwasa, N.; Jung, H. S.; Kato, S.; Kwon, Y. K.; Nishimura, S.; Ota, S.; Setoodehnia, K.; Teranishi, T.; Tokieda, H.; Yamada, T.; Yun, C. C.; Zhang, L. Y.
：: Physical Review C, 巻 97, 番号 1, 015802, 03.01.2018.研究成果: ジャーナルへの寄稿 › 記事
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TY - JOUR
T1 - First measurement of S 30 +α resonant elastic scattering for the S 30 (α,p) reaction rate
AU - Kahl, Daid
AU - Yamaguchi, H.
AU - Kubono, S.
AU - Chen, A. A.
AU - Parikh, A.
AU - Binh, D. N.
AU - Chen, J.
AU - Cherubini, S.
AU - Duy, N. N.
AU - Hashimoto, T.
AU - Hayakawa, S.
AU - Iwasa, N.
AU - Jung, H. S.
AU - Kato, S.
AU - Kwon, Y. K.
AU - Nishimura, S.
AU - Ota, S.
AU - Setoodehnia, K.
AU - Teranishi, T.
AU - Tokieda, H.
AU - Yamada, T.
AU - Yun, C. C.
AU - Zhang, L. Y.
PY - 2018/1/3
Y1 - 2018/1/3
N2 - Background: Type I x-ray bursts are the most frequently observed thermonuclear explosions in the galaxy, resulting from thermonuclear runaway on the surface of an accreting neutron star. The S30(α,p) reaction plays a critical role in burst models, yet insufficient experimental information is available to calculate a reliable, precise rate for this reaction. Purpose: Our measurement was conducted to search for states in Ar34 and determine their quantum properties. In particular, natural-parity states with large α-decay partial widths should dominate the stellar reaction rate. Method: We performed the first measurement of S30+α resonant elastic scattering up to a center-of-mass energy of 5.5 MeV using a radioactive ion beam. The experiment utilized a thick gaseous active target system and silicon detector array in inverse kinematics. Results: We obtained an excitation function for S30(α,α) near 150 in the center-of-mass frame. The experimental data were analyzed with R-matrix calculations, and we observed three new resonant patterns between 11.1 and 12.1 MeV, extracting their properties of resonance energy, widths, spin, and parity. Conclusions: We calculated the resonant thermonuclear reaction rate of S30(α,p) based on all available experimental data of Ar34 and found an upper limit about one order of magnitude larger than a rate determined using a statistical model. The astrophysical impact of these two rates has been investigated through one-zone postprocessing type I x-ray burst calculations. We find that our new upper limit for the S30(α,p)Cl33 rate significantly affects the predicted nuclear energy generation rate during the burst.
AB - Background: Type I x-ray bursts are the most frequently observed thermonuclear explosions in the galaxy, resulting from thermonuclear runaway on the surface of an accreting neutron star. The S30(α,p) reaction plays a critical role in burst models, yet insufficient experimental information is available to calculate a reliable, precise rate for this reaction. Purpose: Our measurement was conducted to search for states in Ar34 and determine their quantum properties. In particular, natural-parity states with large α-decay partial widths should dominate the stellar reaction rate. Method: We performed the first measurement of S30+α resonant elastic scattering up to a center-of-mass energy of 5.5 MeV using a radioactive ion beam. The experiment utilized a thick gaseous active target system and silicon detector array in inverse kinematics. Results: We obtained an excitation function for S30(α,α) near 150 in the center-of-mass frame. The experimental data were analyzed with R-matrix calculations, and we observed three new resonant patterns between 11.1 and 12.1 MeV, extracting their properties of resonance energy, widths, spin, and parity. Conclusions: We calculated the resonant thermonuclear reaction rate of S30(α,p) based on all available experimental data of Ar34 and found an upper limit about one order of magnitude larger than a rate determined using a statistical model. The astrophysical impact of these two rates has been investigated through one-zone postprocessing type I x-ray burst calculations. We find that our new upper limit for the S30(α,p)Cl33 rate significantly affects the predicted nuclear energy generation rate during the burst.
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U2 - 10.1103/PhysRevC.97.015802
DO - 10.1103/PhysRevC.97.015802
M3 - Article
AN - SCOPUS:85040190965
VL - 97
JO - Physical Review C
JF - Physical Review C
SN - 2469-9985
IS - 1
M1 - 015802
ER -