High-resolution study of 37Cl →37Ar Gamow-Teller transition via 37Cl(3He,t)37Ar reaction

Y. Shimbara, Y. Fujita, T. Adachi, G. P.A. Bergc, B. A. Brown, H. Fujimura, H. Fujita, Kunihiro Fujita, K. Hara, K. Y. Hara, K. Hatanaka, J. Kamiya, K. Katori, T. Kawabata, K. Nakanishi, G. Martìnez-Pinedo, N. Sakamotoc, Y. Sakemi, Y. Shimizu, T. Tameshige & 4 others M. Uchida, M. Yoshifuku, M. Yosoi, R. G.T. Zegers

Research output: Chapter in Book/Report/Conference proceedingConference contribution

Abstract

We performed a 37Cl(3He,t)37Ar experiment at E = 140 MeV/nucleon and 0° with a resolution of 30 keV. The Gamow-Teller (GT) strength distribution was obtained up to the excitation energy (E x) of 14.2 MeV in 37Ar. Under the assumption of isospin symmetry, the GT strengths in the 37Cl →37Ar and 37Ca →37K transitions are analogous. The obtained strength distribution was compared with the mirror 37Ca β decay up to Ex = 8.6 MeV. The overall shapes of the distributions were similar, but the details were not necessary the same. In order to understand those differences, the experimental distribution was compared with the shell model (SM) calculation using the USD interaction. The SM calculation suggests that differences at lower energies can be caused by a large tensor contribution in the charge-exchange reaction. On the other hand, the differences seen at higher energies are due to the breaking of the mirror symmetry. The neutrino cross section for the 8B solar neutrino source was calculated using the obtained data.

Original languageEnglish
Title of host publication10th International Symposium on Origin of Matter and Evolution of Galaxies, OMEG10
Pages201-206
Number of pages6
DOIs
Publication statusPublished - Sep 21 2010
Externally publishedYes
Event10th International Symposium on Origin of Matter and Evolution of Galaxies, OMEG10 - Osaka, Japan
Duration: Mar 8 2010Mar 10 2010

Publication series

NameAIP Conference Proceedings
Volume1269
ISSN (Print)0094-243X
ISSN (Electronic)1551-7616

Other

Other10th International Symposium on Origin of Matter and Evolution of Galaxies, OMEG10
CountryJapan
CityOsaka
Period3/8/103/10/10

Fingerprint

high resolution
mirrors
solar neutrinos
symmetry
charge exchange
energy
neutrinos
tensors
cross sections
decay
excitation
interactions

All Science Journal Classification (ASJC) codes

  • Physics and Astronomy(all)

Cite this

Shimbara, Y., Fujita, Y., Adachi, T., Bergc, G. P. A., Brown, B. A., Fujimura, H., ... Zegers, R. G. T. (2010). High-resolution study of 37Cl →37Ar Gamow-Teller transition via 37Cl(3He,t)37Ar reaction. In 10th International Symposium on Origin of Matter and Evolution of Galaxies, OMEG10 (pp. 201-206). (AIP Conference Proceedings; Vol. 1269). https://doi.org/10.1063/1.3485135

High-resolution study of 37Cl →37Ar Gamow-Teller transition via 37Cl(3He,t)37Ar reaction. / Shimbara, Y.; Fujita, Y.; Adachi, T.; Bergc, G. P.A.; Brown, B. A.; Fujimura, H.; Fujita, H.; Fujita, Kunihiro; Hara, K.; Hara, K. Y.; Hatanaka, K.; Kamiya, J.; Katori, K.; Kawabata, T.; Nakanishi, K.; Martìnez-Pinedo, G.; Sakamotoc, N.; Sakemi, Y.; Shimizu, Y.; Tameshige, T.; Uchida, M.; Yoshifuku, M.; Yosoi, M.; Zegers, R. G.T.

10th International Symposium on Origin of Matter and Evolution of Galaxies, OMEG10. 2010. p. 201-206 (AIP Conference Proceedings; Vol. 1269).

Research output: Chapter in Book/Report/Conference proceedingConference contribution

Shimbara, Y, Fujita, Y, Adachi, T, Bergc, GPA, Brown, BA, Fujimura, H, Fujita, H, Fujita, K, Hara, K, Hara, KY, Hatanaka, K, Kamiya, J, Katori, K, Kawabata, T, Nakanishi, K, Martìnez-Pinedo, G, Sakamotoc, N, Sakemi, Y, Shimizu, Y, Tameshige, T, Uchida, M, Yoshifuku, M, Yosoi, M & Zegers, RGT 2010, High-resolution study of 37Cl →37Ar Gamow-Teller transition via 37Cl(3He,t)37Ar reaction. in 10th International Symposium on Origin of Matter and Evolution of Galaxies, OMEG10. AIP Conference Proceedings, vol. 1269, pp. 201-206, 10th International Symposium on Origin of Matter and Evolution of Galaxies, OMEG10, Osaka, Japan, 3/8/10. https://doi.org/10.1063/1.3485135
Shimbara Y, Fujita Y, Adachi T, Bergc GPA, Brown BA, Fujimura H et al. High-resolution study of 37Cl →37Ar Gamow-Teller transition via 37Cl(3He,t)37Ar reaction. In 10th International Symposium on Origin of Matter and Evolution of Galaxies, OMEG10. 2010. p. 201-206. (AIP Conference Proceedings). https://doi.org/10.1063/1.3485135
Shimbara, Y. ; Fujita, Y. ; Adachi, T. ; Bergc, G. P.A. ; Brown, B. A. ; Fujimura, H. ; Fujita, H. ; Fujita, Kunihiro ; Hara, K. ; Hara, K. Y. ; Hatanaka, K. ; Kamiya, J. ; Katori, K. ; Kawabata, T. ; Nakanishi, K. ; Martìnez-Pinedo, G. ; Sakamotoc, N. ; Sakemi, Y. ; Shimizu, Y. ; Tameshige, T. ; Uchida, M. ; Yoshifuku, M. ; Yosoi, M. ; Zegers, R. G.T. / High-resolution study of 37Cl →37Ar Gamow-Teller transition via 37Cl(3He,t)37Ar reaction. 10th International Symposium on Origin of Matter and Evolution of Galaxies, OMEG10. 2010. pp. 201-206 (AIP Conference Proceedings).
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abstract = "We performed a 37Cl(3He,t)37Ar experiment at E = 140 MeV/nucleon and 0° with a resolution of 30 keV. The Gamow-Teller (GT) strength distribution was obtained up to the excitation energy (E x) of 14.2 MeV in 37Ar. Under the assumption of isospin symmetry, the GT strengths in the 37Cl →37Ar and 37Ca →37K transitions are analogous. The obtained strength distribution was compared with the mirror 37Ca β decay up to Ex = 8.6 MeV. The overall shapes of the distributions were similar, but the details were not necessary the same. In order to understand those differences, the experimental distribution was compared with the shell model (SM) calculation using the USD interaction. The SM calculation suggests that differences at lower energies can be caused by a large tensor contribution in the charge-exchange reaction. On the other hand, the differences seen at higher energies are due to the breaking of the mirror symmetry. The neutrino cross section for the 8B solar neutrino source was calculated using the obtained data.",
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AU - Brown, B. A.

AU - Fujimura, H.

AU - Fujita, H.

AU - Fujita, Kunihiro

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AU - Shimizu, Y.

AU - Tameshige, T.

AU - Uchida, M.

AU - Yoshifuku, M.

AU - Yosoi, M.

AU - Zegers, R. G.T.

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N2 - We performed a 37Cl(3He,t)37Ar experiment at E = 140 MeV/nucleon and 0° with a resolution of 30 keV. The Gamow-Teller (GT) strength distribution was obtained up to the excitation energy (E x) of 14.2 MeV in 37Ar. Under the assumption of isospin symmetry, the GT strengths in the 37Cl →37Ar and 37Ca →37K transitions are analogous. The obtained strength distribution was compared with the mirror 37Ca β decay up to Ex = 8.6 MeV. The overall shapes of the distributions were similar, but the details were not necessary the same. In order to understand those differences, the experimental distribution was compared with the shell model (SM) calculation using the USD interaction. The SM calculation suggests that differences at lower energies can be caused by a large tensor contribution in the charge-exchange reaction. On the other hand, the differences seen at higher energies are due to the breaking of the mirror symmetry. The neutrino cross section for the 8B solar neutrino source was calculated using the obtained data.

AB - We performed a 37Cl(3He,t)37Ar experiment at E = 140 MeV/nucleon and 0° with a resolution of 30 keV. The Gamow-Teller (GT) strength distribution was obtained up to the excitation energy (E x) of 14.2 MeV in 37Ar. Under the assumption of isospin symmetry, the GT strengths in the 37Cl →37Ar and 37Ca →37K transitions are analogous. The obtained strength distribution was compared with the mirror 37Ca β decay up to Ex = 8.6 MeV. The overall shapes of the distributions were similar, but the details were not necessary the same. In order to understand those differences, the experimental distribution was compared with the shell model (SM) calculation using the USD interaction. The SM calculation suggests that differences at lower energies can be caused by a large tensor contribution in the charge-exchange reaction. On the other hand, the differences seen at higher energies are due to the breaking of the mirror symmetry. The neutrino cross section for the 8B solar neutrino source was calculated using the obtained data.

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