Photodisintegration of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow /><mml:mrow><mml:mn>9</mml:mn></mml:mrow></mml:msup></mml:mrow><mml:mi mathvariant="normal">Be</mml:mi></mml:math>with laser-induced Compton backscattered<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>γ</mml:mi></mml:math>rays

Utsunomiya, H.; Yonezawa, Yasushige; Akimune, H.; Yamagata, T.; Ohta, M.; Fujishiro, Masatoshi; Toyokawa, Hiroyuki; Ohgaki, Hideaki

doi:10.1103/physrevc.63.018801

Cited by 77 publications

(122 citation statements)

References 22 publications

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“…Many of the details can be found in [14] Experimentally two reaction channels of n + 8 Be and 5 He + α cannot be distinguished.…”

Section: Methodsmentioning

confidence: 99%

“…Recently, Utsunomiya et al made a new measurement of σ γn for 9 Be in the range of E γ = 1.78 -6.11 with quasi-monochromatic γ rays produced by means of inverse Compton scattering of laser photons [14]. The data essentially include all states of astrophysical interest.…”

Section: Resonances Of 9 Bementioning

confidence: 99%

“…Recently, a systematic measurement of the 9 Be(γ,n) 8 Be reaction was made with laser-electron photon beams in the energy range of astrophysical relevance [14]. This study has provided photoneutron cross sections as a function of γ-ray energy.…”

Section: Introductionmentioning

confidence: 99%

“…It is to be noted that we add data points immediately above the neutron threshold since the brief report [14]. We provide the reaction rate in the wide range of temperatures from T 9 =10 −3 to T 9 =10 1 in the analytical fitting formula as well as in the tabular form.…”

Section: Introductionmentioning

confidence: 99%

“…Since the direct measurement of the α(αn, γ) 9 Be reaction is impossible, the experimental efforts to provide information on excited states in 9 Be have been made (see [13,14] and the references therein). A ternary process hardly plays a role in the formation of 9 Be.…”

Section: Introductionmentioning

confidence: 99%

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Astrophysical reaction rate for α(αn,γ)9Be by photodisintegration

et al. 2002

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We study the astrophysical reaction rate for the formation of 9 Be through the three body reaction α(αn, γ). This reaction is one of the key reactions which could bridge the mass gap at A = 8 nuclear systems to produce intermediate-to-heavy mass elements in alpha-and neutron-rich environments such as r-process nucleosynthesis in supernova explosions, s-process nucleosynthesis in asymptotic giant branch (AGB) stars, and primordial nucleosynthesis in baryon inhomogeneous cosmological models. To calculate the thermonuclear reaction rate in a wide range of temperatures, we numerically integrate the thermal average of cross sections assuming a two-steps formation through a metastable 8 Be, α + α ⇀ ↽ 8 Be(n,γ) 9 Be. Off-resonant and on-resonant contributions from the ground state in 8 Be are taken into account. As input cross section, we adopt the latest experimental data by photodisintegration of 9 Be with laser-electron photon beams, which covers all relevant resonances in 9 Be. Experimental data near the neutron threshold are added with γ-ray flux corrections and a new least-squares analysis is made to deduce resonance parameters in the Breit-Wigner formulation. Based on the photodisintegration cross section, we provide the reaction rate for α(αn, γ) 9 Be in the temperature range from T 9 =10 −3 to T 9 =10 1 (T 9 is the temperature in units of 10 9 K) both in the tabular form and in the analytical form for potential usage in nuclear reaction network calculations.The calculated reaction rate is compared with the reaction rates of the CF88 and the NACRE compilations. The CF88 rate, which is based on the photoneutron cross section for the 1/2 + state in 9 Be by Berman et al., is valid at T 9 > 0.028 due to lack of the off-resonant contribution. The CF88 rate differs from the present rate by a factor of two in a temperature range T 9 ≥ 0.1. The NACRE rate, which adopted different sources of experimental information on resonance states in 9 Be, is 4-12 times larger than the present rate at T 9 ≤ 0.028, but is consistent with the present rate to within ±20% at T 9 ≥ 0.1. 2

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“…Many of the details can be found in [14] Experimentally two reaction channels of n + 8 Be and 5 He + α cannot be distinguished.…”

Section: Methodsmentioning

confidence: 99%

Section: Resonances Of 9 Bementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Astrophysical reaction rate for α(αn,γ)9Be by photodisintegration

et al. 2002

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Photonuclear reaction data and γ-ray sources for astrophysics

Utsunomiya¹,

Goko²,

Toyokawa³

et al.

The 2nd International Conference on Nuclear Physics in Astrophysics

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Abstract. Direct determination of photoneutron cross sections of astrophysical importance has recently become possible with use of quasi-monochromatic γ beams produced in laser Compton backscattering (LCS) from relativistic electrons at AIST. The astrophysics to be discussed with the photodisintegration cross section are both stellar and big bang nucleosyntheses regarding the production of p-process and s-process nuclei as well as light elements. Synchrotron radiations from a 10 tesla superconducting wiggler (SCW) at SPring-8 serve as an ideal photon source to determine photoreaction rates. This paper covers the latest cross section measurements with the LCS photon beams and a feasibility study of determining (γ, x) (x = n, p, α) reaction rates with the SCW radiation.

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Nuclear structure effects in the isotope shift with halo nuclei

Puchalski¹,

Pachucki²

2010

Laser 2009

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Photodisintegration of9Bewith laser-induced Compton backscatteredγrays

Cited by 77 publications

References 22 publications

Astrophysical reaction rate for α(αn,γ)9Be by photodisintegration

Astrophysical reaction rate for α(αn,γ)9Be by photodisintegration

Photonuclear reaction data and γ-ray sources for astrophysics

Nuclear structure effects in the isotope shift with halo nuclei

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