Strong-focusing in tandem accelerator with alternating voltage gradient

Sagara, K.; Nakashima, Torahiko; Nakamura, Masafumi; Okuda, Hitoshi; Yagita, T.; Tsuruta, Kenji; Ikeda, Nobuo; Morinobu, S.

doi:10.1016/s0168-9002(01)02063-0

Cited by 8 publications

(8 citation statements)

References 2 publications

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“…However, acceleration voltage in the 12 C+ 4 He experiment is 1-3 MV and the beam transmission is only 5-15%. Therefore, we developed a method called an acceleration-deceleration operation to increase the beam transmission [5]. The beam transmission was increased twice or more by the operation.…”

Section: Methodsmentioning

confidence: 99%

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Direct measurement of 12C+4He→16O+γ total cross section at Ecm=1.2 MeV

Yamaguchi¹,

Sagara²,

Fujita³

et al. 2014

AIP Conference Proceedings

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O+γ is one of the main reactions in He-burning of stars and important for nucleosynthesis. The fusion cross section at stellar energy of E cm = 0.3 MeV has not been determined precisely yet in spite of efforts for about 40 years. We plan to measure directly the total fusion cross section down to 0.7 MeV at Kyushu University Tandem accelerator Laboratory and to estimate the cross section at 0.3MeV by extrapolation. We have already measured the cross sections at 2.4 MeV and 1.5 MeV. The measurement at E cm =1.2 MeV is in progress.

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Section: Methodsmentioning

confidence: 99%

“…Because of the small cross section, a background (BG) reduction is very difficult. The target, a detection system and a method to increase the beam intensity have been developed [5][6][7][8].…”

Section: Introductionmentioning

confidence: 99%

Direct measurement of 12C+4He→16O+γ total cross section at Ecm=1.2 MeV

Yamaguchi¹,

Sagara²,

Fujita³

et al. 2014

AIP Conference Proceedings

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“…The stellar reaction rate is a key input to the star evolution, and many scholars have contributed studies on it. [3−8] At the end of helium burning in a massive star, the main production is 12 C, but 12 C can capture α particles through the reaction channel 12 C(α, γ) 16 O and then form 16 O and emit photons. The 12 C(α, γ) 16 O is a principal reaction which completes during helium burning in a massive star to determine the yields of 12 C and 16 O.…”

Section: Introductionmentioning

confidence: 99%

“…[3−8] At the end of helium burning in a massive star, the main production is 12 C, but 12 C can capture α particles through the reaction channel 12 C(α, γ) 16 O and then form 16 O and emit photons. The 12 C(α, γ) 16 O is a principal reaction which completes during helium burning in a massive star to determine the yields of 12 C and 16 O. The abundance ratio of 12 C and 16 O is the beginning condition of the continuing nuclear process, which has considerable influence on the nucleosynthesis and star evolution of massive stars.…”

Section: Introductionmentioning

confidence: 99%

“…The 12 C(α, γ) 16 O is a principal reaction which completes during helium burning in a massive star to determine the yields of 12 C and 16 O. The abundance ratio of 12 C and 16 O is the beginning condition of the continuing nuclear process, which has considerable influence on the nucleosynthesis and star evolution of massive stars. This abundance ratio of 12 C and 16 O is determined by the astrophysical 12 C(α, γ) 16 O reaction rate, which is an essential input of massive stellar evolution.…”

Section: Introductionmentioning

confidence: 99%

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