Low-lying levels in<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi mathvariant="normal">Cu</mml:mi></mml:mrow><mml:mprescripts /><mml:mrow /><mml:mrow><mml:mn>57</mml:mn></mml:mrow><mml:mrow /><mml:mrow /></mml:mmultiscripts></mml:mrow></mml:math>and the<i>rp</i>process

Zhou, XG; Dejbakhsh, H.; Gagliardi, C. A.; Jiang, Jiping; Trache, L.; Tribble, R. E.

doi:10.1103/physrevc.53.982

Cited by 21 publications

(25 citation statements)

References 10 publications

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“…It demarks the point in the rp-process where the rate of energy generation, and thus X-ray burst luminosity profiles, start to drop. We adopt the rate by Forstner et al (2001), which is based on measurements of the n+ 56 Ni mirror spectroscopic factors (Rehm et al 1998) and level information from Zhou et al (1996).…”

Section: Experiments Based Ratesmentioning

confidence: 99%

The Jina Reaclib Database: Its Recent Updates and Impact on Type-I X-Ray Bursts

Cyburt

Amthor

Ferguson

et al. 2010

ApJS

967

847

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We present results from the JINA REACLIB project, an ongoing effort to maintain a current and accurate library of thermonuclear reaction rates for astrophysical applications. Ongoing updates are transparently documented and version tracked, and any set of rates is publicly available and can be downloaded via a web interface at http://groups.nscl.msu.edu/jina/reaclib/db/. We discuss here our library V1.0, a snapshot of recommended rates for stable and explosive hydrogen and helium burning. We show that the updated reaction rates lead to modest but significant changes in full network, full 1D X-ray burst model calculations, compared to calculations with previously used reaction rate sets. The late time behavior of X-ray burst light curves shows significant changes, suggesting that the previously found small discrepancies between model calculations and observations may be solved with a better understanding of the nuclear input. Our X-ray burst model calculations are intended to serve as a benchmark for future model comparisons and sensitivity studies, as the complete underlying nuclear physics is fully documented and publicly available.

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Section: Experiments Based Ratesmentioning

confidence: 99%

The Jina Reaclib Database: Its Recent Updates and Impact on Type-I X-Ray Bursts

Cyburt

Amthor

Ferguson

et al. 2010

ApJS

967

847

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“…p ͑E, l͒ were calculated in a Woods-Saxon potential with a radius parameter of r 0 1.25 fm and a diffuseness of a 0.65 fm or from R-matrix theory using a radius of 5.36 fm [17]. The excitation energies of these states were determined recently [18].…”

mentioning

confidence: 99%

Study of the56Ni(d,p)57NiReaction and the Astrophysical
Rehm¹,
Borasi²,
Jiang³
et al. 1998
Phys. Rev. Lett.
80
1
39
1
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The single-particle character of states outside the doubly magic (radioactive) nucleus 56 Ni has been determined through a measurement of the ͑d, p͒ neutron transfer reaction using inverse kinematics. From the spectroscopic factors of the low-lying states in 57 Ni, the astrophysically interesting yield for the 56 Ni͑p, g͒ reaction to the mirror nucleus 57 Cu has been calculated, utilizing charge symmetry. The rate for this reaction in the temperature range typical of novae, supernovae, and x-ray bursts is found to be more than 10 times higher than previously assumed. [S0031-9007 (97)05085-0]

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“…The proton separation energy of 57 Cu is merely Sp = 694.87 keV (Audi et al 2003a(Audi et al , 2003b, and so all of its excited states are resonances in this reaction. The authors in Zhou et al (1996) stressed that small changes in the binding and excitation energies lead to significant modifications of the predictions for the synthesis of proton rich isotopes with A > 56 and possibly for the time evolution of cosmic X-ray bursts.…”

Section: Gamow-teller Strength Distributionsmentioning

confidence: 99%

“…The rate of this reaction in the stellar kilns is due almost entirely to the first four resonances (Zhou et al 1996) and particularly very sensitive to the location and structure of the low-lying states in daughter 57 Cu. The pn-QRPA accounted well for these low-lying states in 57 Cu.…”

Section: Gamow-teller Strength Distributionsmentioning

confidence: 99%

“…1. Vieira et al (1976) for the first time probed the structure of 57 Cu in the beta decay of 57 Zn by employing the 40 Ca( 20 Ne, 3n) fusion evaporation reaction and by Zhou et al (1996) in the 1 H( 58 Ni, 57 Cu-γ )2n reaction by using the recoil mass spectrometer MARS at the Texas A&M Cyclotron Institute. Considerable improvements were obtained in Jokinen et al (2002) concerning the quality of the experimental data, in particular with respect to source purity and proton energy resolution.…”

Section: Gamow-teller Strength Distributionsmentioning

confidence: 99%

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Gamow-Teller strength distribution in proton-rich nucleus 57Zn and its implications in astrophysics

Nabi

Rahman

2010

Astrophys Space Sci

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Gamow-Teller (GT) transitions play a preeminent role in the collapse of stellar core in the stages leading to a Type-II supernova. The microscopically calculated GT strength distributions from ground and excited states are used for the calculation of weak decay rates for the core-collapse supernova dynamics and for probing the concomitant nucleosynthesis problem. The B(GT) strength for 57 Zn is calculated in the domain of proton-neutron Quasiparticle Random Phase Approximation (pn-QRPA) theory. No experimental insertions were made (as usually made in other pn-QRPA calculations of B(GT) strength function) to check the performance of the model for proton-rich nuclei. The calculated B(GT) strength distribution is in good agreement with measurements and shows differences with the earlier reported shell model calculation. The pn-QRPA model reproduced the measured low-lying strength for 57 Zn better in comparison to the KB3G interaction used in the large-scale shell model calculation. The stellar weak rates are sensitive to the location and structure of these low-lying states in daughter 57 Cu. The structure of 57 Cu plays a sumptuous role in the nucleosynthesis of proton-rich nuclei. The primary mechanism for producing such nuclei is the rp-process and is believed to be important in the dynamics of the collapsing supermassive stars. Small changes in the binding and excitation energies can lead to significant modifications of the predictions for the synthesis of proton rich isotopes. The β + -decay and electron capture (EC) rates (FFN). The pn-QRPA calculated β + -decay rates are generally in good agreement with the FFN calculation. However at high stellar temperatures the calculated β + -decay rates are almost half of FFN rates. On the other hand, for rp-process conditions, the calculated electron capture (β + -decay) rates are bigger than FFN rates by more than a factor 2 (1.5) and may have interesting astrophysical consequences.

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Low-lying levels inCu57and therpprocess

Cited by 21 publications

References 10 publications

The Jina Reaclib Database: Its Recent Updates and Impact on Type-I X-Ray Bursts

The Jina Reaclib Database: Its Recent Updates and Impact on Type-I X-Ray Bursts

Study of the56Ni(d,p)57NiReaction and the Astrophysical
Rehm¹,
Borasi²,
Jiang³
et al. 1998
Phys. Rev. Lett.
80
1
39
1
View full text Add to dashboard Cite

Gamow-Teller strength distribution in proton-rich nucleus 57Zn and its implications in astrophysics

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Low-lying levels inCu57and therpprocess

Cited by 21 publications

References 10 publications

The Jina Reaclib Database: Its Recent Updates and Impact on Type-I X-Ray Bursts

The Jina Reaclib Database: Its Recent Updates and Impact on Type-I X-Ray Bursts

Study of the56Ni(d,p)57NiReaction and the AstrophysicalRehm1, Borasi2, Jiang3 et al. 1998Phys. Rev. Lett.801391View full textAdd to dashboardCite

Gamow-Teller strength distribution in proton-rich nucleus 57Zn and its implications in astrophysics

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Study of the56Ni(d,p)57NiReaction and the Astrophysical
Rehm¹,
Borasi²,
Jiang³
et al. 1998
Phys. Rev. Lett.
80
1
39
1
View full text Add to dashboard Cite