TY - JOUR
T1 - Stau-catalyzed 6Li production in big-bang nucleosynthesis
AU - Hamaguchi, K.
AU - Hatsuda, T.
AU - Kamimura, M.
AU - Kino, Y.
AU - Yanagida, T. T.
N1 - Funding Information:
T.H., M.K. and Y.K. were partly supported by the Grant-in-Aid of MEXT No. 18540253. Useful discussions with Emiko Hiyama are gratefully acknowledged.
PY - 2007/7/5
Y1 - 2007/7/5
N2 - If the gravitino mass is in the region from a few GeV to a few 10's GeV, the scalar lepton X such as stau is most likely the next lightest supersymmetry particle. The negatively charged and long-lived X- may form a Coulomb bound state (A X-) with a nucleus A and may affect the big-bang nucleosynthesis through catalyzed fusion process. We calculate a production cross section of 6Li from the catalyzed fusion (4He X-) + d → 6Li + X- by solving the Schrödinger equation exactly for three-body system of 4He, d and X. We utilize the state-of-the-art coupled-channel method, which is known to be very accurate to describe other three-body systems in nuclear and atomic reactions. The importance of the use of appropriate nuclear potential and the exact treatment of the quantum tunneling in the fusion process are emphasized. We find that the astrophysical S-factor at the Gamow peak corresponding to T = 10 keV is 0.038 MeV barn. This leads to the 6Li abundance from the catalyzed process as 6Li |CBBN ≃ 4.3 × 10-11 (D / 2.8 × 10-5) ([nX- / s] / 10-16) in the limit of long lifetime of X. Particle physics implication of this result is also discussed.
AB - If the gravitino mass is in the region from a few GeV to a few 10's GeV, the scalar lepton X such as stau is most likely the next lightest supersymmetry particle. The negatively charged and long-lived X- may form a Coulomb bound state (A X-) with a nucleus A and may affect the big-bang nucleosynthesis through catalyzed fusion process. We calculate a production cross section of 6Li from the catalyzed fusion (4He X-) + d → 6Li + X- by solving the Schrödinger equation exactly for three-body system of 4He, d and X. We utilize the state-of-the-art coupled-channel method, which is known to be very accurate to describe other three-body systems in nuclear and atomic reactions. The importance of the use of appropriate nuclear potential and the exact treatment of the quantum tunneling in the fusion process are emphasized. We find that the astrophysical S-factor at the Gamow peak corresponding to T = 10 keV is 0.038 MeV barn. This leads to the 6Li abundance from the catalyzed process as 6Li |CBBN ≃ 4.3 × 10-11 (D / 2.8 × 10-5) ([nX- / s] / 10-16) in the limit of long lifetime of X. Particle physics implication of this result is also discussed.
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U2 - 10.1016/j.physletb.2007.05.030
DO - 10.1016/j.physletb.2007.05.030
M3 - Article
AN - SCOPUS:34250644316
VL - 650
SP - 268
EP - 274
JO - Physics Letters, Section B: Nuclear, Elementary Particle and High-Energy Physics
JF - Physics Letters, Section B: Nuclear, Elementary Particle and High-Energy Physics
SN - 0370-2693
IS - 4
ER -