2019
DOI: 10.1140/epja/i2019-12708-4
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The activation method for cross section measurements in nuclear astrophysics

Abstract: The primary aim of experimental nuclear astrophysics is to determine the rates of nuclear reactions taking place in stars in various astrophysical conditions. These reaction rates are important ingredient for understanding the elemental abundance distribution in our solar system and the galaxy. The reaction rates are determined from the cross sections which need to be measured at energies as close to the astrophysically relevant ones as possible. In many cases the final nucleus of an astrophysically important … Show more

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Cited by 61 publications
(43 citation statements)
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References 221 publications
(393 reference statements)
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“…In the present work the E p = 278 keV resonance strength is measured using an independent method, the activation technique [17]. As an additional result, the strength of the E p = 1058 keV resonance in the 14 N(p, γ ) 15 O reaction is also measured.…”
Section: A the Importance Of The E P = 278 Kev Resonancementioning
confidence: 95%
“…In the present work the E p = 278 keV resonance strength is measured using an independent method, the activation technique [17]. As an additional result, the strength of the E p = 1058 keV resonance in the 14 N(p, γ ) 15 O reaction is also measured.…”
Section: A the Importance Of The E P = 278 Kev Resonancementioning
confidence: 95%
“…As outlined above, the primary aim of the present work was the study of the 91 Zr(p,γ) 92m Nb reaction using the activation method [21]. The cross section was determined based on the off-line detection of the γ-radiation following the β-decay of the reaction product.…”
Section: Investigated Reactionsmentioning
confidence: 99%
“…Measuring the 144 Sm(α, γ ) 148 Gd reaction cross section via the activation technique [30] is specifically challenging due to several reasons [31]. The reaction product 148 Gd (see Fig.…”
Section: The 144 Sm(α γ ) 148 Gd Reactionmentioning
confidence: 99%
“…1) decays with a half-life of 71.10(12) yr [29]. This is a timescale which is usually quoted as unfeasible using the activation technique due to the small expected activity, which requires very efficient and sensitive detection techniques [30]. The widely used γ -ray spectroscopy of transitions between excited states in the daughter nucleus after the decay is not possible in this case because the α decay populates directly the ground state of 144 Sm, leaving no characteristic γ -ray fingerprint.…”
Section: The 144 Sm(α γ ) 148 Gd Reactionmentioning
confidence: 99%