Determination of the astrophysical 13N (p, γ) 14O cross section through the Coulomb dissociation method

T. Motobayashi; T. Takei; S. Kox; C. Perrin; F. Merchez; D. Rebreyend; K. Ieki; H. Murakami; Y. Ando; N. Iwasa; M. Kurokawa; S. Shirato; J. Ruan; T. Ichihara; T. Kubo; N. Inabe; A. Goto; S. Kubono; S. Shimoura; M. Ishihara

doi:10.1016/0370-2693(91)90345-Q

Determination of the astrophysical ¹³N (p, γ) ¹⁴O cross section through the Coulomb dissociation method

T. Motobayashi, T. Takei, S. Kox, C. Perrin, F. Merchez, D. Rebreyend, K. Ieki, H. Murakami, Y. Ando, N. Iwasa, M. Kurokawa, S. Shirato, J. Ruan, T. Ichihara, T. Kubo, N. Inabe, A. Goto, S. Kubono, S. Shimoura, M. Ishihara

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21 Citations (Scopus)

Abstract

The Coulomb dissociation reaction ²⁰⁸Pb(¹⁴O, ¹³N p)²⁰⁸Pb was measured at E_in = 87.5 MeV/u to determine the radiative width Γ_γ of the 1^- state in ¹⁴O at E_ex = 5.17 MeV. This state dominates the radiative capture process ¹³N(p, γ) ¹⁴O, a key reaction in the hot CNO cycle of hydrogen burning in stars. We have deduced Γ_γ = 3.1 ± 0.6 eV with the help of a coupled channel calculation. The validity of the technique was confirmed in the case of the ²⁰⁸Pb(¹³N, ¹²C p)²⁰⁸Pb reaction exciting the 1 2⁺ state in ¹³N whose width is known.

Original language	English
Pages (from-to)	259-263
Number of pages	5
Journal	Physics Letters B
Volume	264
Issue number	3-4
DOIs	https://doi.org/10.1016/0370-2693(91)90345-Q
Publication status	Published - 1991 Aug 1
Externally published	Yes

ASJC Scopus subject areas

Nuclear and High Energy Physics

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10.1016/0370-2693(91)90345-Q

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Motobayashi, T., Takei, T., Kox, S., Perrin, C., Merchez, F., Rebreyend, D., Ieki, K., Murakami, H., Ando, Y., Iwasa, N., Kurokawa, M., Shirato, S., Ruan, J., Ichihara, T., Kubo, T., Inabe, N., Goto, A., Kubono, S., Shimoura, S., & Ishihara, M. (1991). Determination of the astrophysical ¹³N (p, γ) ¹⁴O cross section through the Coulomb dissociation method. Physics Letters B, 264(3-4), 259-263. https://doi.org/10.1016/0370-2693(91)90345-Q

Motobayashi, T, Takei, T, Kox, S, Perrin, C, Merchez, F, Rebreyend, D, Ieki, K, Murakami, H, Ando, Y, Iwasa, N, Kurokawa, M, Shirato, S, Ruan, J, Ichihara, T, Kubo, T, Inabe, N, Goto, A, Kubono, S, Shimoura, S & Ishihara, M 1991, 'Determination of the astrophysical ¹³N (p, γ) ¹⁴O cross section through the Coulomb dissociation method', Physics Letters B, vol. 264, no. 3-4, pp. 259-263. https://doi.org/10.1016/0370-2693(91)90345-Q

@article{b6d17dcc99764ede8bea197856f98248,

title = "Determination of the astrophysical 13N (p, γ) 14O cross section through the Coulomb dissociation method",

abstract = "The Coulomb dissociation reaction 208Pb(14O, 13N p)208Pb was measured at Ein = 87.5 MeV/u to determine the radiative width Γγ of the 1- state in 14O at Eex = 5.17 MeV. This state dominates the radiative capture process 13N(p, γ) 14O, a key reaction in the hot CNO cycle of hydrogen burning in stars. We have deduced Γγ = 3.1 ± 0.6 eV with the help of a coupled channel calculation. The validity of the technique was confirmed in the case of the 208Pb(13N, 12C p)208Pb reaction exciting the 1 2+ state in 13N whose width is known.",

author = "T. Motobayashi and T. Takei and S. Kox and C. Perrin and F. Merchez and D. Rebreyend and K. Ieki and H. Murakami and Y. Ando and N. Iwasa and M. Kurokawa and S. Shirato and J. Ruan and T. Ichihara and T. Kubo and N. Inabe and A. Goto and S. Kubono and S. Shimoura and M. Ishihara",

note = "Funding Information: We would like to thank the staffofthe RIKEN Ring Cyclotron for their help. Discussions with. G. Baur have been very useful from the early stage of this work. We are also grateful to P. Aguer, D. Beumel and C. Wilkin for valuable discussions. This work was supported by the Collaboration Program between RIKEN (Japan) and IN2P3 (France).",

year = "1991",

month = aug,

day = "1",

doi = "10.1016/0370-2693(91)90345-Q",

language = "English",

volume = "264",

pages = "259--263",

journal = "Physics Letters, Section B: Nuclear, Elementary Particle and High-Energy Physics",

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T1 - Determination of the astrophysical 13N (p, γ) 14O cross section through the Coulomb dissociation method

AU - Motobayashi, T.

AU - Takei, T.

AU - Kox, S.

AU - Perrin, C.

AU - Merchez, F.

AU - Rebreyend, D.

AU - Ieki, K.

AU - Murakami, H.

AU - Ando, Y.

AU - Iwasa, N.

AU - Kurokawa, M.

AU - Shirato, S.

AU - Ruan, J.

AU - Ichihara, T.

AU - Kubo, T.

AU - Inabe, N.

AU - Goto, A.

AU - Kubono, S.

AU - Shimoura, S.

AU - Ishihara, M.

N1 - Funding Information: We would like to thank the staffofthe RIKEN Ring Cyclotron for their help. Discussions with. G. Baur have been very useful from the early stage of this work. We are also grateful to P. Aguer, D. Beumel and C. Wilkin for valuable discussions. This work was supported by the Collaboration Program between RIKEN (Japan) and IN2P3 (France).

PY - 1991/8/1

Y1 - 1991/8/1

N2 - The Coulomb dissociation reaction 208Pb(14O, 13N p)208Pb was measured at Ein = 87.5 MeV/u to determine the radiative width Γγ of the 1- state in 14O at Eex = 5.17 MeV. This state dominates the radiative capture process 13N(p, γ) 14O, a key reaction in the hot CNO cycle of hydrogen burning in stars. We have deduced Γγ = 3.1 ± 0.6 eV with the help of a coupled channel calculation. The validity of the technique was confirmed in the case of the 208Pb(13N, 12C p)208Pb reaction exciting the 1 2+ state in 13N whose width is known.

AB - The Coulomb dissociation reaction 208Pb(14O, 13N p)208Pb was measured at Ein = 87.5 MeV/u to determine the radiative width Γγ of the 1- state in 14O at Eex = 5.17 MeV. This state dominates the radiative capture process 13N(p, γ) 14O, a key reaction in the hot CNO cycle of hydrogen burning in stars. We have deduced Γγ = 3.1 ± 0.6 eV with the help of a coupled channel calculation. The validity of the technique was confirmed in the case of the 208Pb(13N, 12C p)208Pb reaction exciting the 1 2+ state in 13N whose width is known.

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Determination of the astrophysical ¹³N (p, γ) ¹⁴O cross section through the Coulomb dissociation method

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