(n, γ) cross-sections of light p nuclei

Nucleosynthesis in the s process takes place in the He burning layers of low mass AGB stars and during the He and C burning phases of massive stars. The s process contributes about half of the element abundances between Cu and Bi in solar system material. Depending on stellar mass and metallicity the resulting s-abundance patterns exhibit characteristic features, which provide comprehensive information for our understanding of the stellar life cycle and for the chemical evolution of galaxies. The rapidly growing body of detailed abundance observations, in particular for AGB and post-AGB stars, for objects in binary systems, and for the very faint metal-poor population represents exciting challenges and constraints for stellar model calculations. Based on updated and improved nuclear physics data for the s-process reaction network, current models are aiming at ab initio solution for the stellar physics related to convection and mixing processes. Progress in the intimately related areas of observations, nuclear and atomic physics, and stellar modeling is reviewed and the corresponding interplay is illustrated by the general abundance patterns of the elements beyond iron and by the effect of sensitive branching points along the sprocess path. The strong variations of the s-process efficiency with metallicity bear also interesting consequences for Galactic chemical evolution.

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“…The Pb data are from ; ; Roederer et al (2009Roederer et al ( , 2008b; . Tables TABLE I MACS (Dillmann et al, 2005), see Sec. II.D).…”

Section: Discussionmentioning

confidence: 99%

“…For easy access, the compilation of Bao et al (2000) was published in electronic form via the KADoNiS project (http://www.kadonis.org) (Dillmann et al, 2005). The current version KADoNiS v0.3 Dy,and 195 Pt, which lie mostly outside the s-process path in the proton-rich p-process domain.…”

Section: Compilations Of Stellar (N γ) Cross Sections and Further Rementioning

confidence: 99%

Thesprocess: Nuclear physics, stellar models, and observations

et al. 2011

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“…A collection of MACSs for all isotopes along the s path is given in Ref. [4] and in the online database KADONIS [35].…”

Section: Maxwellian Averaged Cross Sectionsmentioning

confidence: 99%

TheZr92(n,γ) reaction and its implications for stellar nucleosynthesis

Tagliente¹,

Milazzo²,

Fujii³

et al. 2010

Phys. Rev. C

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Because the relatively small neutron capture cross sections of the zirconium isotopes are difficult to measure, the results of previous measurements are often not adequate for a number of problems in astrophysics and nuclear 0556-2813/2010/81(5)/055801 (9) 055801-1 ©2010 The American Physical Society G. TAGLIENTE et al.PHYSICAL REVIEW C 81, 055801 (2010) technology. Therefore, the 92 Zr(n,γ ) cross section has been remeasured at the CERN n TOF facility, providing a set of improved parameters for 44 resonances in the neutron energy range up to 40 keV. With this information the cross-section uncertainties in the keV region could be reduced to 5% as required for s-process nucleosynthesis studies and technological applications.

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“…The KADNS project [6] is based on these previous compilations and aims to be a regularly updated database. The current version KADNS v0.2 (January 2007) is already the second update and includes -compared to the previous Bao et al compilation [4] -38 updated and 14 new recommended cross sections.…”

Section: Stellar Neutron Capture Compilationsmentioning

confidence: 99%

“…Isotopic abundances were taken from [8]. Recommended cross section were taken from [4] and [6]. Italic values show semi-empirical estimates.…”

Section: P-process Simulations With An Updated Reaction Librarymentioning

confidence: 99%

New stellar (n,γ) cross sections and the "Karlsruhe Astrophysical Database of Nucleosynthesis in Stars"

Dillmann

Plag

Domingo‐Pardo

et al. 2007

Nd2007

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Abstract. Since April 2005 a regularly updated stellar neutron cross section compilation is available online at http://nuclear-astrophysics.fzk.de/kadonis. This online-database is called the "Karlsruhe Astrophysical Database of Nucleosynthesis in Stars" project and is based on the previous Bao et al. compilation from the year 2000. The present version KADNS v0.2 (January 2007) includes recommended cross sections for 280 isotopes between 1 H and 210 Po and 75 semi-empirical estimates for isotopes without experimental information. Concerning stellar (n,γ) cross sections of the 32 stable, proton-rich isotopes produced by the p process experimental information is only available for 20 isotopes, but 9 of them have rather large uncertainties of ≥9%. The first part of a systematic study of stellar (n,γ) cross sections of the p-process isotopes 74 Stellar neutron capture compilationsThe pioneering work for stellar neutron capture cross sections was published in 1971 by Allen and co-workers [1]. In this paper the role of neutron capture reactions in the nucleosynthesis of heavy elements was reviewed and a list of recommended (experimental or semi-empirical) Maxwellian averaged cross sections at kT = 30 keV (MACS30) presented for nuclei between C and Pu.The idea of an experimental and theoretical stellar neutron cross section database was picked up again by Bao and Käppeler [2] for s-process studies. This compilation published in 1987 included cross sections for (n,γ) reactions (between 12 C and 209 Bi), some (n,p) and (n,α) reactions (for 33 Se to 59 Ni), and also (n,γ) and (n, f ) reactions for long-lived actinides. A follow-up compilation was published by Beer et al. in 1992 [3].In the update of 2000 the Bao compilation [4] was extended down to 1 H and -like the original Allen papersemi-empirical recommended values for nuclides without experimental cross section information were added. These estimated values are normalized cross sections derived with the Hauser-Feshbach code NON-SMOKER [5], which account for known systematic deficiencies in the nuclear input of the calculation. Additionally, the database provided stellar enhancement factors and energy-dependent MACS for energies between kT = 5 keV and 100 keV.The KADNS project [6] is based on these previous compilations and aims to be a regularly updated database. The current version KADNS v0.2 (January 2007) is already the second update and includes -compared to the previous Bao et al. compilation [4] -38 updated and 14 new recommended cross sections. The update history can be followed in the section "Logbook". A paper version of KADNS ("v1.0") a Presenting author, e-mail: iris.dillmann@ik.fzk.de is planned for 2008, which also will -like the first Bao compilation from 1987 [2] -include (n,p) and (n,α) reactions for light isotopes and (n,γ) and (n, f ) reactions for longlived actinides at kT = 30 keV. Additionally, a re-calculation of semi-empirical estimates based on the latest experimental results of neighboring nuclides will be performed.2 Systematic st...

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(n, γ) cross-sections of light p nuclei

Cited by 28 publications

References 24 publications

Thesprocess: Nuclear physics, stellar models, and observations

Thesprocess: Nuclear physics, stellar models, and observations

TheZr92(n,γ) reaction and its implications for stellar nucleosynthesis

New stellar (n,γ) cross sections and the "Karlsruhe Astrophysical Database of Nucleosynthesis in Stars"

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