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; K. 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; M. Uchida; M. Yoshifuku; M. Yosoi; R. G.T. Zegers

doi:10.1063/1.3485135

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, K. 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. TameshigeM. Uchida, M. Yoshifuku, M. Yosoi, R. G.T. Zegers

Experimental Particle Physics

Research output: Chapter in Book/Report/Conference proceeding › Conference 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 E_x = 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 language	English
Title of host publication	10th International Symposium on Origin of Matter and Evolution of Galaxies, OMEG10
Pages	201-206
Number of pages	6
DOIs	https://doi.org/10.1063/1.3485135
Publication status	Published - 2010
Event	10th International Symposium on Origin of Matter and Evolution of Galaxies, OMEG10 - Osaka, Japan Duration: Mar 8 2010 → Mar 10 2010

Publication series

Name	AIP Conference Proceedings
Volume	1269
ISSN (Print)	0094-243X
ISSN (Electronic)	1551-7616

Other

Other	10th International Symposium on Origin of Matter and Evolution of Galaxies, OMEG10
Country/Territory	Japan
City	Osaka
Period	3/8/10 → 3/10/10

All Science Journal Classification (ASJC) codes

Physics and Astronomy(all)

Access to Document

10.1063/1.3485135

Cite this

Shimbara, Y., Fujita, Y., Adachi, T., Bergc, G. P. A., Brown, B. A., Fujimura, H., Fujita, H., Fujita, K., Hara, K., Hara, K. Y., Hatanaka, K., Kamiya, J., Katori, K., Kawabata, T., Nakanishi, K., Martìnez-Pinedo, G., Sakamotoc, N., Sakemi, Y., Shimizu, Y., ... 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

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

@inproceedings{946762e0c87f475fb6c71b6e21885401,

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

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.",

author = "Y. Shimbara and Y. Fujita and T. Adachi and Bergc, {G. P.A.} and Brown, {B. A.} and H. Fujimura and H. Fujita and K. Fujita and K. Hara and Hara, {K. Y.} and K. Hatanaka and J. Kamiya and K. Katori and T. Kawabata and K. Nakanishi and G. Mart{\`i}nez-Pinedo and N. Sakamotoc and Y. Sakemi and Y. Shimizu and T. Tameshige and M. Uchida and M. Yoshifuku and M. Yosoi and Zegers, {R. G.T.}",

note = "Copyright: Copyright 2010 Elsevier B.V., All rights reserved.; 10th International Symposium on Origin of Matter and Evolution of Galaxies, OMEG10 ; Conference date: 08-03-2010 Through 10-03-2010",

year = "2010",

doi = "10.1063/1.3485135",

language = "English",

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series = "AIP Conference Proceedings",

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T1 - High-resolution study of 37Cl →37Ar Gamow-Teller transition via 37Cl(3He,t)37Ar reaction

AU - Shimbara, Y.

AU - Fujita, Y.

AU - Adachi, T.

AU - Bergc, G. P.A.

AU - Brown, B. A.

AU - Fujimura, H.

AU - Fujita, H.

AU - Fujita, K.

AU - Hara, K.

AU - Hara, K. Y.

AU - Hatanaka, K.

AU - Kamiya, J.

AU - Katori, K.

AU - Kawabata, T.

AU - Nakanishi, K.

AU - Martìnez-Pinedo, G.

AU - Sakamotoc, N.

AU - Sakemi, Y.

AU - Shimizu, Y.

AU - Tameshige, T.

AU - Uchida, M.

AU - Yoshifuku, M.

AU - Yosoi, M.

AU - Zegers, R. G.T.

PY - 2010

Y1 - 2010

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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U2 - 10.1063/1.3485135

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T3 - AIP Conference Proceedings

SP - 201

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BT - 10th International Symposium on Origin of Matter and Evolution of Galaxies, OMEG10

T2 - 10th International Symposium on Origin of Matter and Evolution of Galaxies, OMEG10

Y2 - 8 March 2010 through 10 March 2010

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