Erratum: Stellar neutron capture cross sections of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mmultiscripts><mml:mi mathvariant="normal">Ne</mml:mi><mml:mprescripts /><mml:none /><mml:mrow><mml:mn>20</mml:mn><mml:mo>,</mml:mo><mml:mn>21</mml:mn><mml:mo>,</mml:mo><mml:mn>22</mml:mn></mml:mrow></mml:mmultiscripts></mml:math>[Phys. Rev. C<b>90</b>, 045804 (2014)]

Heil, M.; Plag, R.; Uberseder, E.; Gallino, R.; Bisterzo, S.; Juseviciute, A.; Käppeler, F.; Lederer, C.; Mengoni, A.; Pignatari, M.

doi:10.1103/physrevc.92.019902

Cited by 3 publications

(3 citation statements)

References 41 publications

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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.

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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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“…It is interesting to note that the higher s-process efficiency found with the reduced MACS data for 23 Na is partly compensated by the effect of revised (n, γ) data for the Ne [46] and Mg [47] isotopes. Accordingly, we confirm the conclusion of Heil et al [46] for the weak component, i.e. that "the reproduction of the s abundances in the solar system is far from being settled."…”

Section: B Massive Starsmentioning

confidence: 99%

Stellar ( n,γ ) cross sections of Na23

et al. 2017

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The cross section of the 23 Na(n, γ) 24 Na reaction has been measured via the activation method at the Karlsruhe 3.7 MV Van de Graaff accelerator. NaCl samples were exposed to quasistellar neutron spectra at kT = 5.1 and 25 keV produced via the 18 O(p, n) 18 F and 7 Li(p, n) 7 Be reactions, respectively. The derived capture cross sections σ kT=5keV = 9.1 ± 0.3 mb and σ kT=25keV = 2.03 ± 0.05 mb are significantly lower than reported in literature. These results were used to substantially revise the radiative width of the first 23 Na resonance and to establish an improved set of Maxwellian average cross sections. The implications of the lower capture cross section for current models of s-process nucleosynthesis are discussed.

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“…The propagation effect due to light neutron poisons was first discussed by Busso & Gallino (1985) for 22 Ne. For more recent discussions see Pignatari et al (2010), and Massimi et al (2012) for 25 Mg and Heil et al (2014) for the Ne isotopes.…”

Section: Nuclear Physics Inputmentioning

confidence: 99%

RE-EVALUATION OF THE¹⁶O(N,γ)¹⁷O CROSS SECTION AT ASTROPHYSICAL ENERGIES AND ITS ROLE AS A NEUTRON POISON IN THEs-PROCESS

Mohr

Heinz

Pignatari

et al. 2016

ApJ

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The doubly-magic nucleus 16 O has a small neutron capture cross section of just a few tens of microbarn in the astrophysical energy region. Despite of this, 16 O plays an important role as neutron poison in the astrophysical slow neutron capture (s) process due to its high abundance. We present in this paper a re-evaluation of the available experimental data for 16 O(n, γ) 17 O and derive a new recommendation for the Maxwellian-averaged cross sections (MACS) between kT = 5−100 keV. Our new recommendations are lower up to kT = 60 keV compared to the previously recommended values but up to 14% higher at kT = 100 keV. We explore the impact of this different energy dependence on the weak s-process during core helium-(kT = 26 keV) and shell carbon burning (kT = 90 keV) in massive stars where 16 O is the most abundant isotope.

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Erratum: Stellar neutron capture cross sections ofNe20,21,22[Phys. Rev. C90, 045804 (2014)]

Cited by 3 publications

References 41 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

Stellar ( n,γ ) cross sections of Na23

RE-EVALUATION OF THE¹⁶O(N,γ)¹⁷O CROSS SECTION AT ASTROPHYSICAL ENERGIES AND ITS ROLE AS A NEUTRON POISON IN THEs-PROCESS

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Erratum: Stellar neutron capture cross sections ofNe20,21,22[Phys. Rev. C90, 045804 (2014)]

Cited by 3 publications

References 41 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

Stellar ( n,γ ) cross sections of Na23

RE-EVALUATION OF THE16O(N,γ)17O CROSS SECTION AT ASTROPHYSICAL ENERGIES AND ITS ROLE AS A NEUTRON POISON IN THEs-PROCESS

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RE-EVALUATION OF THE¹⁶O(N,γ)¹⁷O CROSS SECTION AT ASTROPHYSICAL ENERGIES AND ITS ROLE AS A NEUTRON POISON IN THEs-PROCESS