(<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi mathvariant="normal">He</mml:mi></mml:mrow><mml:mprescripts /><mml:mrow /><mml:mrow><mml:mn>3</mml:mn></mml:mrow><mml:mrow /><mml:mrow /></mml:mmultiscripts></mml:mrow><mml:mo>,</mml:mo><mml:mi>n</mml:mi></mml:math>) Reaction at 25 MeV

Greenfield, M. B.; Bingham, C. R.; Newman, E.; Saltmarsh, M.J.

doi:10.1103/physrevc.6.1756

Cited by 37 publications

(24 citation statements)

References 35 publications

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“…[39] but disagrees slightly with Ref. [54] and with the AME03 value. The Q EC value for the beta decay of 60 Zn [55] is in agreement with the mass excess value measured in this work (see Fig.…”

Section: Zncontrasting

confidence: 56%

“…The studied neutron-deficient nuclides were produced at the Ion-Guide Isotope Separator On-Line (IGISOL) facility [10]. In the first run, proton or 3 He 2+ beams from the K-130 cyclotron impinging on enriched 54 Fe (2 mg/cm 2 ) or 58 Ni (1.8 mg/cm 2 ) targets produced the ions of interest employing the light-ion ion-guide [11]. The corresponding proton beam intensity was about 10 µA and the 3 He 2+ beam 0.5 pµA.…”

Section: Experimental Methodsmentioning

confidence: 99%

“…T 1/2 I π Ex (keV) 56 ton beam was used to test the production of 54 Ni and 56 Cu. However, these exotic nuclides were not observed in this run.…”

Section: Nuclidementioning

confidence: 99%

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Mass measurements in the vicinity of the doubly magic waiting pointNi56

et al. 2010

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Section: Zncontrasting

confidence: 56%

Section: Experimental Methodsmentioning

confidence: 99%

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Mass measurements in the vicinity of the doubly magic waiting pointNi56

et al. 2010

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“…Although dσ (E) dE for 3 He( 28 Si, 30 S) is negative within this energy range [20,21], the combined energy dependence of the momentum straggling within the production target and the emerging charge-state distribution of 30 S more than compensate for the decreasing σ (E); RI beam production and ion-optical transport simulations are consistent with this interpretation of our experimental data. Although dσ (E) dE for 3 He( 28 Si, 30 S) is negative within this energy range [20,21], the combined energy dependence of the momentum straggling within the production target and the emerging charge-state distribution of 30 S more than compensate for the decreasing σ (E); RI beam production and ion-optical transport simulations are consistent with this interpretation of our experimental data.…”

Section: S Beam Productionsupporting

confidence: 82%

[sup 30]S Beam Development and X-ray Bursts

Kahl¹,

Chen²,

Kubono³

et al. 2010

AIP Conference Proceedings

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Over the past three years, we have worked on developing a well-characterized 30 S radioactive beam to be used in a future experiment aiming to directly measure to extrapolate the 30 S(α,p) stellar reaction rate within the Gamow window of Type I X-ray bursts. The importance of the 30 S(α,p) reaction to X-ray bursts is discussed. Given the astrophysical motivation, the successful results of and challenges involved in the production of a low-energy 30 S beam are detailed. Finally, an overview of our future plans regarding this on-going project are presented.The 30 S(α,p) reaction is a significant link in the αp-process, which competes with the rpprocess in Type I X-ray bursts (XRBs) [1], but the reaction rate is virtually unconstrained by experimental data. Not only are there no data directly measuring the 30 S(α,p) cross section in the literature (at any energy), but there are no conclusive experimental reports on the nuclear structure of the compound nucleus 34 Ar above the α-threshold with regard to any possible α-resonances. Hydrodynamic models of XRBs indicate that variation of the theoretical reaction rate has significant consequences.XRBs are understood to result from thermonuclear runaway in the hydrogen-and helium-rich accreted envelopes on the electron-degenerate surfaces of neutron star binary systems [2]. Accretion ensures a steady flow of fresh material will spread around the surface of the neutron star only to be buried by the continuous pile-up of more matter. Equilibrium between a fierce gravitational pressure and the constant energy release of the β -limited CNO cycle is broken by a thin-shell instability, triggering the onset of explosive nucleosynthesis [3,4] . Although powerful, these bursts do not disrupt the binary star system, hence X-ray bursters exhibit recurring episodes with hourly, daily, or more extended regularity, making them the "most common thermonuclear explosions in the universe" [5]. Computer simulations reproduce the energy release, burst profiles (rise time, peak wavelength, and decay curve), and the recurrence time-scales of these astrophysical phenomena.

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“…The neutron deficient 62Zn nucleus has previously been studied by various transfert reactions: (160, 12C) [1], (p, t) [2][3][4][5], (3He, n) [6,7] and (6Li, d) [8] reactions, and J~ assignments up to 4 + have been deduced principally from the DWBA analysis of the (p, t) angular distributions. A few decay 7-rays were also known from the 63Cu(p, 2n7) reaction [4] (assigned from the relative pattern of the excitation function).…”

Section: Introductionmentioning

confidence: 99%

In beam gamma spectroscopy of62Zn

Bruandet¹,

Chan²,

Agard³

et al. 1976

Z Physik A

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The decay scheme of 62Zn has been investigated by studying the yield functions, angular distributions and coincidence relation-ships of the 7-rays emitted in the 63Cu(p, 2n7) and 6~ 2n7) reactions. Spins up to 7 h were assigned to the observed states.Nuclear Reactions. 6~ E~=28-35MeV and 63Cu(p, 2nT)62Zn, Ep= 22-31 MeV; measured Er, I~(0), I~(Ep) and Ir(E~), 7-7 coincidences, 62Zn deduced decay scheme. Enriched target, Ge(Li) detectors.

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(He3,n) Reaction at 25 MeV

Cited by 37 publications

References 35 publications

Mass measurements in the vicinity of the doubly magic waiting pointNi56

Mass measurements in the vicinity of the doubly magic waiting pointNi56

[sup 30]S Beam Development and X-ray Bursts

In beam gamma spectroscopy of62Zn

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