Gamow-Teller decay of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi mathvariant="normal">Zn</mml:mi></mml:mrow><mml:mprescripts /><mml:mrow /><mml:mrow><mml:mn>80</mml:mn></mml:mrow><mml:mrow /><mml:mrow /></mml:mmultiscripts></mml:mrow></mml:math>: Shell structure and astrophysical implications

Kratz, Karl; Harms, V.; Wöhr, A.; Möller, P.

doi:10.1103/physrevc.38.278

Cited by 26 publications

(16 citation statements)

References 20 publications

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“…However, for the A_~80 r-abundance peak the opposite effect may occur. The initial odd-even staggering of the progenitor abundances arising from the odd-even effects in the neutron binding energies (for discussion of this point, see, e.g., [29,30]), may be further enhanced by the odd-even staggering in delayed neutron branching around 26<Z_<33, N-~50 [14,28,36]. Hence, /?-delayed neutron emission seems to be a possible nuclear-structure explanation of the unusually pronounced odd-even effect in the solar r-abundances of VSAs to 8SRb [27,37].…”

Section: Astrophysical Implicationsmentioning

confidence: 98%

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Calculation of beta-decay properties of neutron-rich nickel isotopes

Kratz

Pfeiffer

Wöhr

et al. 1989

Z. Physik A - Atomic Nuclei

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Section: Astrophysical Implicationsmentioning

confidence: 98%

“…First results of this systematic study have been discussed in [13,14]. In this paper, we present model calculations for neutron-rich zaNi isotopes which are -or may soon become accessible to experiment.…”

Section: Introductionmentioning

confidence: 99%

Calculation of beta-decay properties of neutron-rich nickel isotopes

Kratz

Pfeiffer

Wöhr

et al. 1989

Z. Physik A - Atomic Nuclei

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“…As was discussed in detail in Ref. [17], agreement between the nuclearphysics prediction of T1/~ and the astrophysical request (approximate equality of Nr,p/T1/2 for all "waiting-point" nuclei) could only be obtained when assuming a small pn(S~ and a large Pn(79Cu). With the known Nr, | of S~ and 799r, the measured T1/2 and Pn of s~ and the experimental P~(79Cu), the "waiting-point" request for the T1/2 of 79Cu is: …”

mentioning

confidence: 93%

Neutron-rich isotopes around the r-process ?waiting-point? nuclei 29 79 Cu50 and 30 80 Zn50

Kratz

Gabelmann

Möller³

et al. 1991

Z. Physik A - Hadrons and Nuclei

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Abstract. Beta-decay half-lives (T1/~) and delayed-neutron emission probabilities (P~) of very neutron-rich Cu to As nuclei have been measured, among them the new isotopes r Cu4s, 79Cuso, mZnsl and S4Ga~a. With the T1/2 and P~-vaIues of now four N ~-50 "waiting-point" nuclei known, our hypothesis that the r-process has attained a local [3-flow equilibrium araound A ~_ 80 is further strengthened.The nucleosynthesis process by rapid neutron captures (the r-process) involves the progressive build-up of heavy elements via neutron captures on neutron-rich nuclei, interspersed by ~-decays. Its abundance features (see, e.g., Ref.[1]) clearly reflect nuclear properties -the maxima are related to the magic neutron numbers N = 50, 82 and 126. This probes our knowledge of nuclear structure of isotopes very far from the valley of fl-stability, even through the postion of the neutron drip line. For the vast majority of nuclei in or close to the r-process path, no experimental information is available; hence, nuclear properties have to be deduced from theoretical models. However, since even the most recent QRPA-predictions [2,3] differ up to an order of magnitude far off stability, it remains of utmost importance to continue experimental efforts to measure the T1/2 and Pn-values of at least the key-isotopes in the r-process path. And in fact, only within the last few years has it been possible to determine these gross decay properties of a few nuclei in the bends at N = 50 and 82 where the r-process path comes closest to/3-stability [4][5][6][7].Based on these data, together with QRPA shell-model predictions for unknown N -50 and 82 r-process isotopes, strong evidence has been obtained that the solar r-abundances (Nr,| result from a ~-fiow equilibrium [6,7]. Within this "waitingpoint" concept, it was possible to define stellar conditions which an r-process has to fulfill in order to reproduce the "correct" process path around the magic neutron numbers, as well as the observed A _~ 80 and 130 Nr,| An additional test was performed for the unknown N = 50 and 82 "waitingpoint" nuclei. From the Nr, | of stable isobars and known (or predicted) Pn-values, progenitor abundances (N~,p) in the rprocess path were calculated; and with this also the T1/2 of these isotopes were "predicted". Although these astrophysical * Dedicated to P. Armbruster on the occasion of his 60th birthday T1/2 requirements were found to agree closely with the nuclearphysics values (see the T1D(QRPA ) in Tab. 1 of Ref. [7]), a final decision whether our steady-flow picture holds can only be made from further experiments on "waiting-point" nuclei.Recently, as a result of extensive target/ion-source tests at the CEI~N-ISOLDE on-line mass separator, considerable progress could be achieved in the production of intense beams of neutron-rich isotopes of 29Cu to a3As. In these experiments, a 2ssUC-graphite target was irradiated with 600 MeV protons at a current of 2.2 #A from the synchro-cyclotron. The target was heated to about 2.400~ and connected to a plasmadischarge...

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“…Early β-decay results seem to indicate a substantial shell quenching [35], while in-beam experiments on N ∼ 50 Ge-Se isotopes [36] and isomer studies following fragmentation [37,38,39,40] give evidence for the persistence of the N = 50 shell. Decisive for both the Z = 28 and N = 50 shell gaps in 78 Ni is according to the tensor force scenario sketched on the right hand side of fig.…”

Section: From 48 Ca To 78 Nimentioning

confidence: 99%

Nuclear structure far off stability --Implications for nuclear astrophysics

Grawe¹,

Blazhev

Górska³

et al. 2006

Eur. Phys. J. A

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Abstract. The single-particle structure and shell gap of 100 Sn as inferred from previous in-beam γ-ray spectroscopy has been confirmed in recent studies of seniority and spin-gap isomers by γγ, βγ, βpγ, pγ and 2pγ spectroscopy. The results for 94,95 Ag, 98 Cd and its N = 50 isotones 96 Pd and 94 Ru stress the importance of large-scale shell model calculations employing realistic interactions for the isomerism, np-nh excitations, seniority mixing and E2 polarisation of the 100 Sn core. The strong monopole interaction of the ∆l = 0, 1 spin/isospin-flip partners πg 9/2 -νg 7/2 along the N = 50 isotones and the πf 5/2 -νg 9/2 pair of nucleons along the Z = 28 Ni isotopes are decisive for the evolution of the shell structure towards 100 Sn and 78 Ni. It can be traced back to the tensor force in the effective nucleon-nucleon interaction and provides a straightforward explanation for new shells in neutron-rich light nuclei, implying qualitative predictions for new N = 32, 34 subshells in Ca isotopes, persistence of the 78 Ni proton and neutron shell gaps and non-equivalence of the g 9/2 valence mirror Ni isotopes and N = 50 isotones. This is corroborated by recent experimental data on 56,58 Cr and 70-76 Ni. The implication of monopole driven shell evolution for apparent spin-orbit splitting towards N Z and structure along the astrophysical r-path between N = 50 and N = 82 is discussed.

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Gamow-Teller decay ofZn80: Shell structure and astrophysical implications

Cited by 26 publications

References 20 publications

Calculation of beta-decay properties of neutron-rich nickel isotopes

Calculation of beta-decay properties of neutron-rich nickel isotopes

Neutron-rich isotopes around the r-process ?waiting-point? nuclei 29 79 Cu50 and 30 80 Zn50

Nuclear structure far off stability --Implications for nuclear astrophysics

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