Erratum:<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mmultiscripts><mml:mi>Ni</mml:mi><mml:mprescripts/><mml:none/><mml:mn>62</mml:mn></mml:mmultiscripts><mml:mo>(</mml:mo><mml:mrow><mml:mi>n</mml:mi><mml:mo>,</mml:mo><mml:mi>γ</mml:mi><mml:mo>)</mml:mo></mml:mrow></mml:math>and<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mmultiscripts><mml:mi>Ni</mml:mi><mml:mprescripts/><mml:none/><mml:mn>63</mml:mn></mml:mmultiscripts><mml:mo>(</mml:mo><mml:mrow><mml:mi>n</mml:mi><mml:m

Lederer, C.; Massimi, C.; Berthoumieux, E.; Colonna, N.; Dressler, R.; Guerrero, C.; Gunsing, F.; Käppeler, F.; Kivel, N.; Pignatari, M.; Reifarth, R.; Schumann, D.; Wallner, A.; Altstadt, S.; Andriamonje, S.; Andrzejewski, J.; Audouin, L.; Barbagallo, M.; Bécares, V.; Bečvář, F.; Belloni, F.; Berthier, B.; Billowes, J.; Boccone, V.; Bosnar, D.; Brügger, M.; Calviani, M.; Calviño, F.; Cano‐Ott, D.; Carrapiço, C.; Cerutti, F.; Chiaveri, E.; Chin, M.; Cortés, G.; Cortés‐Giraldo, M. A.; Dillmann, I.; Domingo‐Pardo, C.; Durán, I.; Dzysiuk, N.; Eleftheriadis, C.; Fernández‐Ordóñez, M.; Ferrari, A.; Fraval, K.; Ganesan, S.; Garcia, A.; Giubrone, G.; Gómez-Hornillos, M.B.; Gonçalves, I. F.; González‐Romero, E.; Gramegna, F.; Griesmayer, E.; Gurusamy, P.; Harrisopulos, S.; Heil, M.; Ioannides, K. G.; Jenkins, D. G.; Jericha, E.; Kadi, Y.; Karadimos, D.; Korschinek, G.; Krtička, M.; Kroll, J.; Langer, C.; Lebbos, E.; Leeb, H.; Leong, L.S.; Losito, R.; Lozano, M.; Manousos, A.; Marganiec, J.; Marrone, S.; Martı́nez, T.; Mastinu, P.; Mastromarco, M.; Meaze, M.; Mendoza, E.; Mengoni, A.; Milazzo, P. M.; Mingrone, F.; Mirea, M.; Mondalaers, W.; Paradela, C.; Pavlik, A.; Perkowski, J.; Plag, R.; Plompen, A.; Praena, J.; Quesada, J. M.; Rauscher, T.; Riego, A.; Román, F.; Rubbia, C.; Sarmento, R.; Schillebeeckx, P.; Schmidt, S.; Tagliente, G.; Taı́n, J. L.; Tarrío, D.; Tassan‐Got, L.; Tsinganis, A.; Tlustos, L.; Valenta, S.; Vannini, G.; Variale, V.; Vaz, P.; Ventura, A.; Vermeulen, M. J.; Versaci, R.; Vlachoudis, V.; Vlastou, R.; Ware, T.; Weigand, M.; Weiß, Christoph; Wright, T.; Žugec, P.

doi:10.1103/physrevc.92.019903

Cited by 5 publications

(2 citation statements)

References 37 publications

(55 reference statements)

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“…Compared to Pi13, for the present work we have adopted an updated nuclear reaction network, including a few different neutron capture reaction rates. In particular, for this work we used the new cross sections for neutron captures on 20,21,22 Ne by Heil et al (2014), 62,63 Ni by Lederer et al (2014), and90,91,92,93,94,95,96 Zr (Tagliente et al 2012;Lugaro et al 2014, and references therein). The only exception is model M3.z2m2.st, that was calculated using the same nuclear reaction network of Pi13.…”

Section: Appendix: Impact Of the New Mesa Revision And Of The New Nucmentioning

confidence: 99%

Application of a Theory and Simulation-Based Convective Boundary Mixing Model for Agb Star Evolution and Nucleosynthesis

Battino¹,

Pignatari²,

Ritter³

et al. 2016

ApJ

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112

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The s-process nucleosynthesis in Asymptotic Giant Branch (AGB) stars depends on the modeling of convective boundaries. We present models and s-process simulations that adopt a treatment of convective boundaries based on the results of hydrodynamic simulations and on the theory of mixing due to gravity waves in the vicinity of convective boundaries. Hydrodynamics simulations suggest the presence of convective boundary mixing (CBM) at the bottom of the thermal pulse-driven convective zone. Similarly, convection-induced mixing processes are proposed for the mixing below the convective envelope during third dredge-up where the 13 C pocket for the s process in AGB stars forms. In this work we apply a CBM model motivated by simulations and theory to models with initial mass M = 2 and M = 3M , and with initial metal content Z = 0.01 and Z = 0.02. As reported previously, the He-intershell abundance of 12 C and 16 O are increased by CBM at the bottom of pulse-driven convection zone. This mixing is affecting the 22 Ne(α,n) 25 Mg activation and the s-process efficiency in the 13 C-pocket. In our model CBM at the bottom of the convective envelope during the third dredgeup represents gravity wave mixing. We take further into account that hydrodynamic simulations indicate a declining mixing efficiency already about a pressure scale height from the convective boundaries, compared to mixing-length theory. We obtain the formation of the 13 C-pocket with a mass of ≈ 10 −4 M . The final s-process abundances are characterized by 0.36 < [s/Fe] < 0.78 and the heavy-to-light s-process ratio is −0.23 < [hs/ls] < 0.45. Finally, we compare our results with stellar observations, pre-solar grain measurements and previous work.

show abstract

Section: Appendix: Impact Of the New Mesa Revision And Of The New Nucmentioning

confidence: 99%

Application of a Theory and Simulation-Based Convective Boundary Mixing Model for Agb Star Evolution and Nucleosynthesis

Battino¹,

Pignatari²,

Ritter³

et al. 2016

ApJ

Self Cite

112

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show abstract

“…The full (dotted) line corresponds to the TALYS calculation obtained with the D1M+QRPA+0lim dipole strength obtained with C = 3 · 10 −8 MeV −3 (C = 10 −7 MeV −3 ). Experimental data are taken from[45][46][47][48][49][50]. The hashed areas correspond to the prediction uncertainties associated with different nuclear level density models.…”

mentioning

confidence: 99%

Photoneutron cross sections for Ni isotopes: Toward understanding (n,γ) cross sections relevant to weak s -process nucleosynthesis

et al. 2018

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Photoneutron cross sections were measured for 58 Ni, 60 Ni, 61 Ni, and 64 Ni at energies between the one-neutron and two-neutron thresholds using quasi-monochromatic γ-ray beams produced in laser Compton-scattering at the NewSUBARU synchrotron radiation facility. The new photoneutron data are used to extract the γ-ray strength function above the neutron threshold complementing the information obtained by the Oslo method below the threshold. We discuss radiative neutron capture cross sections and the Maxwellian-averaged cross sections for Ni isotopes including 63 Ni, a branching point nucleus along the weak s-process path. The cross sections are calculated with the experimentally constrained γ-ray strength functions from the Hartree-Fock-Bogolyubov plus quasiparticle-random phase approximation based on the Gogny D1M interaction for both E1 and M 1 components and supplemented with the M 1 upbend.

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Neutron-induced cross section measurements

et al. 2023

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Neutron-induced cross sections represent the main nuclear input to models of stellar and Big-Bang nucleosynthesis. While (n,γ) reactions are relevant for the formation of elements heavier than iron, (n,p) and (n,α) reactions can play an important role in specific cases. The time-of-flight method is routinely used at n_TOF to experimentally determine the cross section data. In addition, recent upgrades of the facility will allow the use of activation techniques as well, possibly opening the way to a systematic study of neutron interaction with radioactive isotopes. In the last 20 years n_TOF has provided a large amount of experimental data for Nuclear Astrophysics. Our plan is to carry on challenging measurements and produce nuclear data in the next decades as well.

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Erratum:Ni62(n,γ)andNi63(n

Cited by 5 publications

References 37 publications

Application of a Theory and Simulation-Based Convective Boundary Mixing Model for Agb Star Evolution and Nucleosynthesis

Application of a Theory and Simulation-Based Convective Boundary Mixing Model for Agb Star Evolution and Nucleosynthesis

Photoneutron cross sections for Ni isotopes: Toward understanding (n,γ) cross sections relevant to weak s -process nucleosynthesis

Neutron-induced cross section measurements

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