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Alford, W.P.; Brown, B. A.; Burzyński, Stanisław; Celler, Anna; Frekers, D.; Helmer, R. L.; Henderson, R.; Jackson, K. P.; Lee, K.; Rahav, A.; Trudel, A.; Vetterli, M. C.

doi:10.1103/physrevc.48.2818

Cited by 68 publications

(64 citation statements)

References 19 publications

(16 reference statements)

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“…It is also remarkable the similarity of the GT strength distributions of the various excited states. Experimental measurements from (n,p) [31] and (d, 2 He) [32] reactions are also shown in the case 51 V. The GT strength appears concentrated at around 5 MeV, whereas the calculations predict the bump at somewhat larger energies. The total GT strength measured in both experiments is quite similar and agrees with the calculations.…”

Section: A Gamow-teller Strength Distributionsmentioning

confidence: 92%

“…The calculations correspond to QRPA results with SLy4 Skyrme force. Data from different charge-exchange reaction experiments [30][31][32][33] are also shown when available.…”

Section: A Gamow-teller Strength Distributionsmentioning

confidence: 99%

“…1. There is also experimental information [30][31][32][33] on the GT strength distributions in 45 Sc, 51 V, and 55 Mn obtained from charge-exchange reactions that will be used for comparison.…”

Section: Introductionmentioning

confidence: 99%

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Contribution of excited states to stellar weak-interaction rates in odd-Anuclei

Sarriguren¹

2016

Phys. Rev. C

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Weak-interaction rates, including β decay and electron capture, are studied in several odd-A nuclei in the pf -shell region at various densities and temperatures of astrophysical interest. Special attention is paid to the relative contribution to these rates of thermally populated excited states in the decaying nucleus. The nuclear structure involved in the weak processes is studied within a quasiparticle random-phase approximation with residual interactions in both particle-hole and particle-particle channels on top of a deformed Skyrme Hartree-Fock mean field with pairing correlations. In the range of densities and temperatures considered, it is found that the total rates do not differ much from the rates of the ground state fully populated. In any case, the changes are not larger than the uncertainties due to the nuclear-model dependence of the rates.

show abstract

Section: A Gamow-teller Strength Distributionsmentioning

confidence: 92%

“…The calculations correspond to QRPA results with SLy4 Skyrme force. Data from different charge-exchange reaction experiments [30][31][32][33] are also shown when available.…”

Section: A Gamow-teller Strength Distributionsmentioning

confidence: 99%

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Contribution of excited states to stellar weak-interaction rates in odd-Anuclei

Sarriguren¹

2016

Phys. Rev. C

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“…FFN estimated their rates based upon the presence of a single Gamow-Teller (GT) resonance which they derived on the basis of the independent particle model, supplemented, where available, by experimental data for low-lying transitions. However, recent experimental data on the GT distributions in nuclei (Alford et al 1990 ;Vetterli et al 1989 ;Alford et al 1993 ;El-Kateb et al 1994 ; Williams et al 1990) shows a quenching of the total GT strength compared to the independent-particle model value. More importantly, the data also show a fragmentation of the GT strength over many states in the daughter nucleus.…”

Section: The New Ratesmentioning

confidence: 99%

Presupernova Evolution with Improved Rates for Weak Interactions

Heger

Woosley

Martı́nez-Pinedo

et al. 2001

ApJ

210

228

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Recent shell-model calculations of weak-interaction rates for nuclei in the mass range A \ 45È65 have resulted in substantial revisions to the hitherto standard set of Fuller, Fowler, & Newman (FFN). In particular, key electron-capture rates, such as that for 60Co, are much smaller. We consider here the e †ects of these revised rates on the presupernova (postÈoxygen burning) evolution of massive stars in the mass range 11È40Moreover, we include, for the Ðrst time in models by our group, the e †ects of M _ . modern rates for beta decay in addition to electron capture and positron emission. Stars of 15, 25, and 40 are examined in detail using both the full FFN rate set and the revised rates. An additional M _ Ðnely spaced (in mass) grid of 34 models is also calculated in order to give the systematics of iron core and silicon core masses. Values for the central electron mole number at the time of iron core collapse in the new models are typically larger, by than those of Woosley & Weaver, with a *Y e \ 0.005È0.015, tendency for the more massive models to display larger di †erences. About half of this change is a consequence of including beta decay ; the other half, the result of the smaller rates for electron capture. Unlike what might be expected solely on basis of the larger values, the new iron core masses are systemati-Y e cally smaller owing to a decrease in the entropy in the outer iron core. The changes in iron core mass range from zero to 0.1 (larger changes for high-mass stars). It would be erroneous however to esti-M _ mate the facility of exploding these new models based solely upon their iron core mass since the entire core structure is altered and the density change is not so di †erent as the adjustments in composition might suggest. We also observe, as predicted by Aufderheide et al., a tendency toward beta equilibrium just prior to the collapse of the core, and the subsequent loss of that equilibrium as core collapse proceeds. This tendency is more pronounced in the 15 model than in the heavier stars. We discuss the M _ key weak reaction rates, both beta decay and electron capture, responsible for the evolution of and Y e make suggestions for future measurements.

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“…To [20,21]. The B(GT) value of these transition is listed in Table I, along with ground state β-decay.…”

Section: Previous Work On Thementioning

confidence: 99%

β -decay rate of Fe59 in shell burning environment and its influence on the production of Fe60
Li
¹
,
Lam
²
,
Qi
³

et al. 2016
Phys. Rev. C
8
0
7
0
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We deduced the stellar β-decay rate of 59 Fe at typical carbon shell burning temperature by taking the experimental Gamow-Teller transition strengths of the 59 Fe excited states. The result is also compared with those derived from large-scale shell model calculation. The new rate is up to a factor of 2.5 lower than theoretical rate of Fuller-Fowler-Newman (FFN) and up to a factor of 5 higher than decay rate of Langanke and Martínez-Pinedo (LMP) in temperature region of 0.5≤T [GK]≤2. We estimated the impact of the newly determined rate on the synthesis of cosmic γ emitter 60 Fe in the C-shell burning and explosive C/Ne burning using one-zone model calculation. Our results show that 59 Fe stellar β−decay plays an important role in the 60 Fe nucleosynthesis, even though the uncertainty of the decay rate is rather large due to the error of B(GT) strengths.

show abstract

Spin-isospin strength distributions inf-pshell nuclei: A study of theV51(n,p) and

Cited by 68 publications

References 19 publications

Contribution of excited states to stellar weak-interaction rates in odd-Anuclei

Contribution of excited states to stellar weak-interaction rates in odd-Anuclei

Presupernova Evolution with Improved Rates for Weak Interactions

β -decay rate of Fe59 in shell burning environment and its influence on the production of Fe60
Li
¹
,
Lam
²
,
Qi
³

et al. 2016
Phys. Rev. C
8
0
7
0
View full text Add to dashboard Cite

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Spin-isospin strength distributions inf-pshell nuclei: A study of theV51(n,p) and

Cited by 68 publications

References 19 publications

Contribution of excited states to stellar weak-interaction rates in odd-Anuclei

Contribution of excited states to stellar weak-interaction rates in odd-Anuclei

Presupernova Evolution with Improved Rates for Weak Interactions

β -decay rate of Fe59 in shell burning environment and its influence on the production of Fe60Li1, Lam2, Qi3 et al. 2016Phys. Rev. C8070View full textAdd to dashboardCite

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About

β -decay rate of Fe59 in shell burning environment and its influence on the production of Fe60
Li
¹
,
Lam
²
,
Qi
³

et al. 2016
Phys. Rev. C
8
0
7
0
View full text Add to dashboard Cite