Structure of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mmultiscripts><mml:mi mathvariant="normal">Na</mml:mi><mml:mprescripts /><mml:none /><mml:mrow><mml:mn>26</mml:mn></mml:mrow></mml:mmultiscripts></mml:math>from the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mmultiscripts><mml:mi mathvariant="normal">C</mml:mi><mml:mprescripts /><mml:none /><mml:mrow><mml:mn>14</mml:mn></mml:mrow></mml:mmultiscripts></mml:math>(<mml:math xmlns:mml="

Lee, Sang-Jin; Tabor, S. L.; Baldwin, Tamara; Campbell, D. B.; Calderin, I. J.; Chandler, C.; Cooper, M. W.; Hoffman, C. R.; Kemper, K. W.; Pavan, J.; Pipidis, A.; Riley, M. A.; Wiedeking, M.

doi:10.1103/physrevc.73.044321

Cited by 31 publications

(38 citation statements)

References 17 publications

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“…The weighted average of the half-life was found to be 192(4) ms, which is in good agreement with previous work [18]. In addition, a weak γ -ray at 2219(4) keV was found which could be the γ -ray transition at 2232(15) keV in 26 Na observed in nuclear reaction studies by Lee et al [19]. The γ -ray at 1996 keV reported in the same work [19] was not seen, although both γ rays were reported to deexcite the same energy level.…”

Section: Ne Analysissupporting

confidence: 86%

“…In addition, a weak γ -ray at 2219(4) keV was found which could be the γ -ray transition at 2232(15) keV in 26 Na observed in nuclear reaction studies by Lee et al [19]. The γ -ray at 1996 keV reported in the same work [19] was not seen, although both γ rays were reported to deexcite the same energy level. The emission probability of the 84 keV γ -ray was not determined because of the high threshold of some of the SeGA detectors, thus this value was adopted from Ref.…”

Section: Ne Analysismentioning

confidence: 73%

“…The comparison of both decay schemes shows reasonable agreement between our data and the shell model calculations. However, Lee et al [19] have argued that older shell model calculations clearly disagree below 3 MeV with the experimental results of the β decay of 26 Ne from the work of Weissman et al based on the nonobservation of a 1 + state in 26 Na predicted to have a relatively strong β branch. They also supported their argument by providing a similar situation in the β decay of 28 Ne.…”

Section: Ne Analysismentioning

confidence: 94%

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Structure ofF23via β decay ofO23

et al. 2007

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The nuclear states in 23 F have been investigated following the β decay of 23 O. The measurement of 23 O was carried out at the National Superconducting Cyclotron Laboratory using fragments from the reaction of a 48 Ca beam in a Be target. The half-life and total neutron emission probability were determined to be 97(8) ms and 7(2)%, respectively, for 23 O β decay. Ten γ -ray decays in 23 F and a single γ -ray in 22 F were observed to establish the β decay scheme for 23 O. Shell model calculations are in reasonable agreement with the measured β branching and B(GT) values for the lowest energy state. The excitation energies of the first 1/2 + and 3/2 + states have been determined to be 2243(8) and 4066(16) keV, respectively, indicating a widening of the 5/2 + -1/2 + state gap in 23 F. The decay scheme of the largest contaminant 26 Ne in the experiment was established.

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Section: Ne Analysissupporting

confidence: 86%

Section: Ne Analysismentioning

confidence: 73%

Section: Ne Analysismentioning

confidence: 94%

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Structure ofF23via β decay ofO23

et al. 2007

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“…A consequence of this is a different (time-evolving) relation between the gravitational potential and the overdensity field; and it is not clear how mechanism was incorporated in the derivation presented by Olivares, Atrio-Brandela & Pavon (2008). Other observational channels which have been considered to constrain energy exchange between dark matter and dark energy are cluster counts (Oguri et al 2003;Manera & Mota 2006;Sutter & Ricker 2008), the CMB (Lee, Liu & Ng 2006), or gravitational lensing (Schäfer, Caldera Cabral & Maartens 2008;La Vacca & Colombo 2008) or supernovae (Gong & Chen 2008).…”

Section: Introductionmentioning

confidence: 99%

The integrated Sachs-Wolfe effect in cosmologies with coupled dark matter and dark energy

Schäfer

2008

Monthly Notices of the Royal Astronomical Society

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The subject of this paper is the derivation of the integrated Sachs–Wolfe (iSW) effect in cosmologies with coupled dark matter and dark energy fluids. These couplings influence the iSW effect in three ways: the Hubble function assumes a different scaling, the structure growth rate shows a different time evolution and, in addition, the Poisson equation, which relates the density perturbations to fluctuations in the gravitational potential, is changed, due to the violation of the scaling ρ∝a−3 of the matter density ρ with scalefactor a. Exemplarily, I derive the iSW spectra for a model in which dark matter decays into dark energy, investigate the influence of the dark matter decay rate and the dark energy equation of state on the iSW signal, and discuss the analogies for gravitational lensing. Quite generally, iSW measurements should reach similar accuracy in determining the dark energy equation of state parameter and the coupling constant.

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“…The sodium isotopes are in the midst of this shell evolution, and therefore play a key role in understanding the nature of this tensor force [11]. Previous β decay studies have shown 26 Na to have a 3 + ground state, and with the exception of a low-lying quartet of states identified by Sangjin Lee et al [12], the structure of 26 Na was largely unknown prior to this work. The (d, p) reaction offers an opportunity to selectively populate and study states with a predominately single-particle structure, which is ideal for measuring the systematic changes of the shell gaps in this region of the Segrè chart.…”

Section: Introductionmentioning

confidence: 90%

Investigating Single-Particle Structure in ²⁶Na Using the New SHARC Array

Wilson¹,

Catford²,

Diget³

et al. 2015

Proceedings of the Conference on Advances in Radioactive Isotope Science (ARIS2014)

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The changing of the nuclear shells for light, neutron-rich nuclei, and the single-particle nature of 26 Na, has been explored by studying 25 Na(d, p) 26 Na in inverse kinematics, using a beam of 25 Na ions at 5 MeV per nucleon, provided by the ISAC-II facility at TRIUMF, Vancouver. Charged particles were detected with a highly-segmented silicon array that surrounded the 0.5 mg/cm 2 (CD 2 ) n target. Gamma rays from the recoiling 26 Na nucleus were detected using eight Compton-suppressed HPGe clover detectors. Recoil tagging was provided by an in-beam scintillation foil, downstream of the germanium array. A novel technique of utilising pγ-and pγγ-gating to extract proton angular distributions from states populated close in energy was employed with success. New states in 26 Na that are populated directly have been identified, using γ-decay patterns. Shell model calculations for comparison to experimental results are ongoing, using different model bases.

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Structure ofNa26from theC14(
Sang-Jin Lee
¹
,
S. L. Tabor
²
,
Tamara Baldwin
³

et al.

Cited by 31 publications

References 17 publications

Structure ofF23via β decay ofO23

Structure ofF23via β decay ofO23

The integrated Sachs-Wolfe effect in cosmologies with coupled dark matter and dark energy

Investigating Single-Particle Structure in ²⁶Na Using the New SHARC Array

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Structure ofNa26from theC14(Sang-Jin Lee1, S. L. Tabor2, Tamara Baldwin3 et al.

Cited by 31 publications

References 17 publications

Structure ofF23via β decay ofO23

Structure ofF23via β decay ofO23

The integrated Sachs-Wolfe effect in cosmologies with coupled dark matter and dark energy

Investigating Single-Particle Structure in 26Na Using the New SHARC Array

Contact Info

Product

Resources

About

Structure ofNa26from theC14(
Sang-Jin Lee
¹
,
S. L. Tabor
²
,
Tamara Baldwin
³

et al.

Investigating Single-Particle Structure in ²⁶Na Using the New SHARC Array