Radiative neutron capture cross sections on<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mmultiscripts><mml:mi>Lu</mml:mi><mml:mprescripts /><mml:none /><mml:mn>176</mml:mn></mml:mmultiscripts></mml:math>at DANCE

Roig, O.; Jändel, M.; Méot, V.; Bond, E. M.; Couture, A.; Haight, R. C.; Keksis, A.; Rundberg, R. S.; Ullmann, J. L.; Vieira, D.J.

doi:10.1103/physrevc.93.034602

Cited by 13 publications

(2 citation statements)

References 35 publications

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“…The IMF averaged production factor is however below 0.2. 176 Lu can be explained with the main s-process in AGB-stars and subject of current experimental efforts (Roig et al 2016). The case of 176 Lu is further complicated by a short-lived 1 − excited state at 122 keV above the 7 − ground state that β decays with a half-life of 3.7 h. The short lived isomer is likely to be populated thermally under supernova conditions and since we do not include it explicitly in our calculations we expect that our results overestimate the yield of 176 Lu.…”

Section: Further Effects On Stable Isotopesmentioning

confidence: 99%

The ν-Process in the Light of an Improved Understanding of Supernova Neutrino Spectra

Sieverding

Martı́nez-Pinedo

Huther

et al. 2018

ApJ

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We study the neutrino-induced production of nuclides in explosive supernova nucleosynthesis for progenitor stars with solar metallicity including neutrino nucleus reactions for all nuclei with charge numbers Z < 76 with average neutrino energies in agreement with modern Supernova simulations. Considering progenitors with initial main sequence masses between 13 M and 30 M , we find a significant production of 11 B, 138 La, and 180 Ta by neutrino nucleosynthesis, despite the significantly reduced neutrino energies. The production of 19 F turns out to be more sensitive to the progenitor mass and structure than to the ν process. With our complete set of cross sections we have identified effects of the ν process on several stable nuclei including 33 S, 40 Ar, 41 K, 59 Co, and 113 In at the 10% level. Neutrino-induced reactions contribute to a similar extent to the production of radioactive 26 Al and increase the yield of 22 Na by 50%. Future γ ray astronomy missions may reach the precision at which the contribution from the ν process becomes relevant. We find that the production of 22 Na by the ν process could explain the Ne-E(L) component of meteoritic graphite grains. The ν process enhances the yield of 36 Cl and we point out that the resulting 36 Cl/ 35 Cl ratio is in agreement with the values infrerred for the early solar system. Our extended set of neutrino-nucleus interactions also allows us to exclude any further effects of the ν process on stable nuclei and to quantify the effects on numerous, hitherto unconsidered radioactive nuclei, e.g., 36 Cl, 72 As, 84 Rb, and 88 Y.

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Section: Further Effects On Stable Isotopesmentioning

confidence: 99%

The ν-Process in the Light of an Improved Understanding of Supernova Neutrino Spectra

Sieverding

Martı́nez-Pinedo

Huther

et al. 2018

ApJ

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“…The full black line shows the predictions obtained adding on top of the defaut prescriptions a low energy M1 strength without any normalization (G norm = 1). Experimental data are taken from references [34][35][36]. Fig.…”

Section: The Compound Nucleus Modelmentioning

confidence: 99%

Potential sources of uncertainties in nuclear reaction modeling

Hilaire

Bauge

Huu-Tai

et al. 2018

EPJ Nuclear Sci. Technol.

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Nowadays, reliance on nuclear models to interpolate or extrapolate between experimental data points is very common, for nuclear data evaluation. It is also well known that the knowledge of nuclear reaction mechanisms is at best approximate, and that their modeling relies on many parameters which do not have a precise physical meaning outside of their specific implementations in nuclear model codes: they carry both specific physical information, and effective information that is related to the deficiencies of the model itself. Therefore, to improve the uncertainties associated with evaluated nuclear data, the models themselves must be refined so that their parameters can be rigorously derived from theory. Examples of such a process will be given for a wide sample of models like: detailed theory of compound nucleus decay through multiple nucleon or gamma emission, or refinements to the width fluctuation factor of the Hauser-Feshbach model. All these examples will illustrate the reduction in the effective components of nuclear model parameters, through the reduced dynamics of parameter adjustment needed to account for experimental data. The significant progress, recently achieved for the non-fission channels, also highlights the difficult path ahead to improve our quantitative understanding of fission in a similar way: by relying on microscopic theory.

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The Production of Therapeutic Radionuclides

Cingoranelli,

Lapi

2023

Radiopharmaceutical Therapy

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Radiative neutron capture cross sections onLu176at DANCE

Cited by 13 publications

References 35 publications

The ν-Process in the Light of an Improved Understanding of Supernova Neutrino Spectra

The ν-Process in the Light of an Improved Understanding of Supernova Neutrino Spectra

Potential sources of uncertainties in nuclear reaction modeling

The Production of Therapeutic Radionuclides

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