Determination of the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mmultiscripts><mml:mi mathvariant="normal">Ce</mml:mi><mml:mprescripts /><mml:none /><mml:mn>142</mml:mn></mml:mmultiscripts></mml:math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mo>(</mml:mo><mml:mi>γ</mml:mi><mml:mo>,</mml:mo><mml:mi>n</mml:mi><mml:mo>)</mml:mo></mml:mrow></mml:math>cross section using quasi-monoenergetic Compton backscattered<mml:math xmlns:mml="http://www.w3.org/1998/Math/Math

Sauerwein, A.; Sonnabend, K.; Fritzsche, M.; Glorius, J.; Kwan, E.; Pietralla, N.; Romig, C.; Rusev, G.; Savran, D.; Schnorrenberger, L.; Tonchev, A. P.; Tornow, W.; Weller, H. R.

doi:10.1103/physrevc.89.035803

Cited by 14 publications

(8 citation statements)

References 41 publications

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“…This method is called photon tagging and can in principle be used to determine the reaction cross sections as a function of γ-energy [205]. Alternatively, photons can be produced by Compton scattering: High-energy electrons interact with laser light and transfer energy via inverse Compton effect [206].…”

Section: Experimental Techniquesmentioning

confidence: 99%

The production of proton-rich isotopes beyond iron: The γ-process in stars

Pignatari

Göbel

Reifarth

et al. 2016

Int. J. Mod. Phys. E

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Beyond iron, a small fraction of the total abundances in the Solar System is made of proton-rich isotopes, the p nuclei. The clear understanding of their production is a fundamental challenge for nuclear astrophysics. The p nuclei constrain the nucleosynthesis in core-collapse and thermonuclear supernovae. The γ process is the most established scenario for the production of the p nuclei, which are produced via different photodisintegration paths starting on heavier nuclei. A large effort from nuclear physics is needed to access the relevant nuclear reaction rates far from the valley of stability. This review describes the production of the heavy proton-rich isotopes by the γ process in stars, and explores the state of the art of experimental nuclear physics to provide nuclear data for stellar nucleosynthesis.

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Section: Experimental Techniquesmentioning

confidence: 99%

The production of proton-rich isotopes beyond iron: The γ-process in stars

Pignatari

Göbel

Reifarth

et al. 2016

Int. J. Mod. Phys. E

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“…In a few experiments, neutrons emitted from the CN were detected and the (γ,n) cross sections were determined. Hauser-Feshbach calculations of these photo-neutron reactions were carried out and comparisons with the data were utilized to determine the most appropriate combination of level densities and γ-ray strength functions [28,30]. These were subsequently employed to calculate the (n,γ) cross section of interest.…”

Section: Methods and Illustrative Examplementioning

confidence: 99%

Compound-nuclear reactions with unstable nuclei: Constraining theory through innovative experimental approaches

Escher

Tonchev

Burke

et al. 2016

EPJ Web of Conferences

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Abstract. Cross sections for compound-nuclear reactions involving unstable targets are important for many applications, but can often not be measured directly. Several indirect methods have recently been proposed to determine neutron capture cross sections for unstable isotopes. We consider three approaches that aim at constraining statistical calculations of capture cross sections with data obtained from the decay of the compound nucleus relevant to the desired reaction. Each method produces this compound nucleus in a different manner (via a light-ion reaction, a photon-induced reaction, or β-decay) and requires additional ingredients to yield the sought-after cross section. We give a brief outline of the approaches and employ preliminary results from recent measurements to illustrate the methods. We discuss the main advantages and challenges of each approach.

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“…7. As shown, the γ-strength function is now fully constrained at all photon energies relevant to the s process by our experimental data, below and above the neutron-separation energy [24]. The experimental γ-ray strength function, obtained by both the (γ,n) [23] and the (γ,γ') measurements [22], was directly included in the TALYS code [28], in a tabulated and interpolated form, for calculating the neutron capture cross section of 85 Kr.…”

Section: Indirect Neutron Capture Cross-section Measurement On Unstabmentioning

confidence: 99%

Nuclear Structure Studies with Gamma-Ray Beams

Tonchev

Bhatia

Kelley

et al. 2015

EPJ Web of Conferences

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Abstract. In stable and weakly bound neutron-rich nuclei, a resonance-like concentration of dipole states has been observed for excitation energies below the neutron-separation energy. This clustering of strong dipole states has been named the Pygmy Dipole Resonance (PDR) in contrast to the Giant Dipole Resonance (GDR) that dominates the E1 response. Understanding the PDR is presently of great interest in nuclear structure and nuclear astrophysics. High-sensitivity studies of E1 and M1 transitions in closed-shell nuclei using monoenergetic and 100% linearly-polarized photon beams are presented.

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Determination of theCe142(γ,n)cross section using quasi-monoenergetic Compton backscattered
A. Sauerwein
¹
,
K. Sonnabend
²
,
M. Fritzsche
³

et al.

Cited by 14 publications

References 41 publications

The production of proton-rich isotopes beyond iron: The γ-process in stars

The production of proton-rich isotopes beyond iron: The γ-process in stars

Compound-nuclear reactions with unstable nuclei: Constraining theory through innovative experimental approaches

Nuclear Structure Studies with Gamma-Ray Beams

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Determination of theCe142(γ,n)cross section using quasi-monoenergetic Compton backscatteredA. Sauerwein1, K. Sonnabend2, M. Fritzsche3 et al.

Cited by 14 publications

References 41 publications

The production of proton-rich isotopes beyond iron: The γ-process in stars

The production of proton-rich isotopes beyond iron: The γ-process in stars

Compound-nuclear reactions with unstable nuclei: Constraining theory through innovative experimental approaches

Nuclear Structure Studies with Gamma-Ray Beams

Contact Info

Product

Resources

About

Determination of theCe142(γ,n)cross section using quasi-monoenergetic Compton backscattered
A. Sauerwein
¹
,
K. Sonnabend
²
,
M. Fritzsche
³

et al.