Measurement of 73Ge(n,γ) cross sections and implications for stellar nucleosynthesis

Lederer-Woods, C.; Battino, U.; Ferreira, Paulo Ricardo Araújo; Gawlik, A.; Guerrero, C.; Gunsing, F.; Heinitz, S.; Lerendegui-Marco, J.; Mengoni, A.; Reifarth, R.; Tattersall, A.; Valenta, S.; Weiß, C.; Aberle, O.; Andrzejewski, J.; Audouin, L.; Bécares, V.; Bacak, M.; Balibrea, J.; Barbagallo, M.; Barros, S.; Bečvář, F.; Beinrucker, C.; Belloni, F.; Berthoumieux, E.; Billowes, J.; Bosnar, D.; Brügger, M.; Caamaño, M.; Calviño, F.; Calviani, M.; Cano‐Ott, D.; Cerutti, F.; Chiaveri, E.; Colonna, N.; Cortés, G.; Cortés‐Giraldo, M. A.; Coséntino, L.; Damone, L. A.; Deo, K.; Diakaki, Μ.; Dietz, M.; Domingo‐Pardo, C.; Dressler, R.; Dupont, E.; Durán, I.; Fernández–Domínguez, B.; Ferrari, A.; Finocchiaro, P.; Frost, R.J.W.; Furman, V.; Göbel, K.; García, A. R.; Gheorghe, I.; Glodariu, T.; Gonçalves, I. F.; González‐Romero, E.; Goverdovski, A.; Griesmayer, E.; Harada, Hideo; Heftrich, T.; Hernández-Prieto, A.; Heyse, J.; Jenkins, D. G.; Jericha, E.; Käppeler, F.; Kadi, Y.; Katabuchi, T.; Kavrigin, P.; Ketlerov, V.; Khryachkov, V.; Kimura, Akira; Kivel, N.; Knapová, I.; Kokkoris, M.; Krtička, M.; Leal-Cidoncha, E.; Leeb, H.; Licata, M.; Meo, S. Lo; Losito, R.; Macina, D.; Marganiec, J.; Martínez, T.; Massimi, C.; Mastinu, P.; Mastromarco, M.; Matteuccí, F.; Mendoza, E.; Milazzo, Paolo; Mingrone, F.; Mirea, M.; Montesano, S.; Musumarra, A.; Nolte, R.; Pinto, Rogelio Palomo; Paradela, C.; Patronis, N.; Pavlik, A.; Perkowski, J.; Porras, I.; Praena, J.; Quesada, J. M.; Rauscher, T.; Riego, A.; Robles, M.; Rubbia, C.; Ryan, J. A.; Sabaté-Gilarte, M.; Saxena, A.; Schillebeeckx, P.; Schmidt, S.; Schumann, D.; Sedyshev, P.; Smith, A. G.; Stamatopoulos, A.; Suryanarayana, S. V.; Tagliente, G.; Taín, J. L.; Tarifeño-Saldivia, A.; Tassan‐Got, L.; Tsinganis, A.; Vannini, G.; Variale, V.; Vaz, P.; Ventura, A.; Vlachoudis, V.; Vlastou, R.; Wallner, A.; Warren, S.; Weigand, M.; Wright, T.; Žugec, P.

doi:10.1016/j.physletb.2019.01.045

Cited by 12 publications

(16 citation statements)

References 27 publications

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“…Using the same method as in Ref. [12], namely the maximum likelihood fit assuming a Gaussian distribution of γ values, we obtained γ = 205(12) meV and σ γ = 70 (10). Our value of the average radiative width is compatible with the literature values 185(30) meV [36] and 185(50) meV [37].…”

Section: Resonance Analysissupporting

confidence: 86%

“…Maxwellian averaged cross sections were calculated and are in very good agreement with the only other previous measurement of this reaction at stellar energies [15], providing an important independent confirmation of stellar cross sections used in astrophysical calculations. The new MACSs combined with recent results for MACSs on 73 Ge(n, γ ) [12] were used to calculate abundances produced in two massive star models, with subsolar and close-to-solar metallicity. Abundances for s-only isotopes match reasonably well with solar system values, in particular for the model close to solar metallicity, while the z = 0.006 model reproduces the germanium isotopic abundance pattern in our solar system.…”

Section: Discussionmentioning

confidence: 99%

“…We have calculated s-process nucleosynthesis abundances for a massive 25M star for two initial metallicities, below solar (z = 0.006) and close to solar metallicity (z = 0.01), 1 using the multizone post-processing code MPPNP [42]. The neutron capture network, which is largely based on rates recommended in the latest released version of KADoNiS, KADoNiS-v0.3 [39], included the new 70 Ge(n, γ ) MACSs obtained in this work and recent results from 73 Ge(n, γ ) [12]. Due to the very good agreement with previous results, there 6.…”

Section: Stellar Cross Sections and Astrophysical Implicationsmentioning

confidence: 99%

“…Existing experimental data on stellar neutron capture on germanium isotopes are scarce, which motivated a campaign at n_TOF to measure cross sections on all stable germanium isotopes [14]. Results on 73 Ge(n, γ ) have recently been published and show that the germanium isotopic abundance pattern produced in the s process in a low metallicity massive star is consistent with the isotopic abundance pattern of our solar system [12]. This paper describes the study of the 70 Ge(n, γ ) reaction.…”

mentioning

confidence: 93%

“…The reaction 70 Ge(n, γ ) has been identified as a key reaction determining the uncertainty of 70 Ge in the main s process, both in the thermal pulse and in interpulse burning of AGB stars [11]. The reaction 70 Ge(n, γ ) and the recently measured 73 Ge(n, γ ) [12] were found to be key reactions for the abundances of 70 Ge and 73 Ge, respectively, in the enhanced weak s process occurring in rotating, metal-poor massive stars [13]. 73 Ge(n, γ ) also appeared as key rate in the regular weak s process in the same study.…”

mentioning

confidence: 99%

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Measurement of the Ge70(n,γ) cross section up to 300 keV at the CERN n_TOF facility

Gawlik¹,

Lederer-Woods²,

Andrzejewski³

et al. 2019

Phys. Rev. C

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Neutron capture data on intermediate mass nuclei are of key importance to nucleosynthesis in the weak component of the slow neutron capture processes, which occurs in massive stars. The (n, γ) cross section on 70 Ge, which is mainly produced in the s process, was measured at the neutron time-of-flight facility n_TOF at CERN. Resonance capture kernels were determined up to 40 keV neutron energy and average cross sections up to 300 keV. Stellar cross sections were calculated from kT = 5 keV to kT = 100 keV and are in very good agreement with a previous measurement by Walter and Beer (1985) and recent evaluations. Average cross sections are in agreement with Walter and Beer (1985) over most of the neutron energy range covered, while they are systematically smaller for neutron energies above 150 keV. We have calculated isotopic abundances produced in s-process environments in a 25 solar mass star for two initial metallicities (below solar and close to solar). While the low metallicity model reproduces best the solar system germanium isotopic abundances, the close to solar model shows a good global match to solar system abundances in the range of mass numbers A = 60-80.

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Section: Resonance Analysissupporting

confidence: 86%

Section: Discussionmentioning

confidence: 99%