(<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>p</mml:mi><mml:mo>,</mml:mo><mml:mi>t</mml:mi></mml:math>) Reaction on Even-Even<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>N</mml:mi><mml:mo>=</mml:mo><mml:mi>Z</mml:mi></mml:math>Nuclei in the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mn>2</mml:mn><mml:mi>s</mml:mi><mml:mn>1</mml:mn><mml:mi>d</mml:mi></mml:math>Shell

Paddock, R.A.

doi:10.1103/physrevc.5.485

Cited by 67 publications

(40 citation statements)

References 37 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The majority of works [15, 16, 18, 20-22, 24, 26] adopted the old value of S p = 5518 keV or something close to it; several [27,29,30,32,33] adopted the newer value of 5513.7 keV from Ref. [37], a 4.3 keV difference; the remainder adopted differing values (5517 [17], 5513 [19], 5512.3 [25,28], and the AME2012 value of 5513.8 [6]) or do not mention any value for S p [13,14].…”

Section: Reanalysis Of Published Datamentioning

confidence: 99%

See 1 more Smart Citation

Resonances above the proton threshold inSi26

Chipps

2016

Phys. Rev. C

View full text Add to dashboard Cite

Section: Reanalysis Of Published Datamentioning

confidence: 99%

“…Only a few measurements were not included in the average, one due to known background issues in the data (Ref. [13]) and the other due to the inability to definitively assign the measured value to a single resonance (Ref. [26]).…”

Section: Adopted Valuesmentioning

confidence: 99%

Resonances above the proton threshold inSi26

Chipps

2016

Phys. Rev. C

View full text Add to dashboard Cite

“…Weighted averages of excitation energies were calculated for the resonances at 289 keV Bardayan et al 2007), 412 keV , 734 keV (Yokota et al 1982;Kuhlmann et al 1973;Setoodehnia et al 2011), 819 keV Fynbo et al 2000;Paddock 1972), 915 keV (Yokota et al 1982;Setoodehnia et al 2010;Paddock 1972), 993 keV (Fynbo et al 2000;Setoodehnia et al 2010;Yokota et al 1982;Paddock 1972). This was unnecessary for resonances at 769 keV ) and 1443 keV (Fynbo et al 2000).…”

Section: C2mentioning

confidence: 99%

STARLIB: A next-generation reaction-rate library for nuclear astrophysics

Sallaska¹,

Iliadis²,

Chapmagne³

et al. 2013

Proceedings of XII International Symposium on Nuclei in the Cosmos — PoS(NIC XII)

View full text Add to dashboard Cite

STARLIB is a next-generation, all-purpose nuclear reaction-rate library. For the first time, this library provides the rate probability density at all temperature grid points for convenient implementation in models of stellar phenomena. The recommended rate and its associated uncertainties are also included. Currently, uncertainties are absent from all other rate libraries, and, although estimates have been attempted in previous evaluations and compilations, these are generally not based on rigorous statistical definitions. A common standard for deriving uncertainties is clearly warranted. STARLIB represents a first step in addressing this deficiency by providing a tabular, up-to-date database that supplies not only the rate and its uncertainty but also its distribution. Because a majority of rates are lognormally distributed, this allows the construction of rate probability densities from the columns of STARLIB. This structure is based on a recently suggested Monte Carlo method to calculate reaction rates, where uncertainties are rigorously defined. In STARLIB, experimental rates are supplemented with: (1) theoretical TALYS rates for reactions for which no experimental input is available, and (2) laboratory and theoretical weak rates. STARLIB includes all types of reactions of astrophysical interest to Z = 83, such as (p, γ ), (p, α), (α, n), and corresponding reverse rates. Strong rates account for thermal target excitations. Here, we summarize our Monte Carlo formalism, introduce the library, compare methods of correcting rates for stellar environments, and discuss how to implement our library in Monte Carlo nucleosynthesis studies. We also present a method for accessing STARLIB on the Internet and outline updated Monte Carlo-based rates.

show abstract

“…Since a direct measurement of the 25 Al(p,γ) 26 Si reaction is presently untenable due to insufficiently intense beams of 25 Al, transfer reactions and in-beam gamma-ray spectroscopic studies have been used extensively to determine indirectly the important level properties of 26 Si, such as resonance energies and spin-parity assignments [1,[11][12][13][14][15][16][17][18][19][20][21][22][23][24][25]. The rate has been re-evaluated recently [23,[26][27][28], and Ref.…”

Section: Introductionmentioning

confidence: 99%