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Jung, Matthias; Bosch, F.; Beckert, K.; Eickhoff, H.; Folger, H.; Franzke, B.; Gruber, A.; Kienle, Paul; Klepper, O.; Koenig, W.; Kozhuharov, C.; Mann, R.C.; Moshammer, R.; Nolden, F.; Schaaf, U.; Soff, G.; Spädtke, P.; Steck, M.; Stöhlker, Th.; Sümmerer, K.

doi:10.1103/physrevlett.69.2164

Cited by 214 publications

(45 citation statements)

References 16 publications

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“…This is notably the case for 163 Dy. A storage-ring experiment at GSI has confirmed that the half-life of fully-ionized 163 Dy +66 is 47 d [248], in excellent agreement with the theoretical prediction of 50 d [247]. Bound-state βdecay can also dramatically modify the terrestrial half-lives of 187 Re and of 205 Pb.…”

Section: Bound-state β − Decayssupporting

confidence: 66%

“…In particular, that mechanism is expected to have a considerable impact on the 187 Re -187 Os cosmochronology (Sect.8.2.3). On the other hand, bound-state β-decay may be used as a tool to determine unknown βdecay matrix elements influencing the design of a 205 Tl neutrino detector [250,251], and perhaps even to set some meaningful limits on the electron neutrino mass [248,252].…”

Section: Bound-state β − Decaysmentioning

confidence: 99%

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Nuclear astrophysics

Arnould¹,

Takahashi²

1999

Rep. Prog. Phys.

167

267

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Nuclear astrophysics is that branch of astrophysics which helps understanding the Universe, or at least some of its many faces, through the knowledge of the microcosm of the atomic nucleus. It attempts to find as many nuclear physics imprints as possible in the macrocosm, and to decipher what those messages are telling us about the varied constituent objects in the Universe at present and in the past. In the last decades much advance has been made in nuclear astrophysics thanks to the sometimes spectacular progress made in the modelling of the structure and evolution of the stars, in the quality and diversity of the astronomical observations, as well as in the experimental and theoretical understanding of the atomic nucleus and of its spontaneous or induced transformations. Developments in other sub-fields of physics and chemistry have also contributed to that advance. Notwithstanding the accomplishment, many longstanding problems remain to be solved, and the theoretical understanding of a large variety of observational facts needs to be put on safer grounds. In addition, new questions are continuously emerging, and new facts endangering old ideas.This review shows that astrophysics has been, and still is, highly demanding to nuclear physics in both its experimental and theoretical components. On top of the fact that large varieties of nuclei have to be dealt with, these nuclei are immersed in highly unusual environments which may have a significant impact on their static properties, the diversity of their transmutation modes, and on the probabilities of these modes. In order to have a chance of solving some of the problems nuclear astrophysics is facing, the astrophysicists and nuclear physicists are obviously bound to put their competence in common, and have sometimes to benefit from the help of other fields of physics, like particle physics, plasma physics or solid-state physics. Given the highly varied and complex aspects, we pick here some specific nuclear physics topics which largely pervade nuclear astrophysics. Direct cross-section measurements 7.3.2. Indirect cross-section measurements 7.4. Neutron capture reactions: Experiments 7.5. Thermonuclear reaction rates: Models 7.5.1. Microscopic models 7.5.2. The potential and DWBA models 7.5.3. Parameter fits 7.5.4. The statistical models 8. Selected topics 8.1. Heavy-element nucleosynthesis by the s-and r-processes of neutron captures 8.1.1. Defining the s-process 8.1.2. Defining the r-process 8.1.3. The s-and r-process contributions to the solar-system composition 8.1.4. Astrophysical sites for the s-and r-processes 8.1.5. Heavy elements in low-metallicity stars 8.2. Cosmochronometry 8.2.1. Nucleo-cosmochronology: generalities 8.2.2. The trans-actinide clocks 8.2.3. The 187 Re -187 Os chronometry 8.3. Type-II supernovae 8.3.1. Evolution of massive stars leading to neutrino-driven supernovae 8.3.2. Nucleosynthesis in the hot bubble: Can the r-process occur ? 8.3.3. Signatures of a large-scale mixing of nucleosynthesis products 9. Summary References * The situ...

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Section: Bound-state β − Decayssupporting

confidence: 66%

Section: Bound-state β − Decaysmentioning

confidence: 99%

Nuclear astrophysics

Arnould¹,

Takahashi²

1999

Rep. Prog. Phys.

167

267

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“…Presently, the most important application of storage rings to nuclear astrophysics has been the determination of bound-β-decay lifetimes. An ingenuous experiment performed with the heavy-ion storage ring ESR at GSI/Darmstadt measured the βdecay half-life of bare 163 Dy [15]. The 163 Dy 66+ ions were stored and accumulated in the ring.…”

Section: Cosmochronometrymentioning

confidence: 99%

Nuclear astrophysics in storage rings

Bertulani

1997

Nuclear Physics A

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Nuclear reaction cross sections are usually very small in typical astrophysical environments. It has been one of the major challenges of experimental nuclear astrophysics to assess the magnitude of these cross sections in the laboratory. For a successful experiment high luminosity beams are needed. Increasing the target width, one also increases the reaction yields. But, this is of limited use due to multiple scattering in the target. Storage rings are a very good way to overcome these difficulties. In principle, they can be tuned to large luminosities, and have the advantage of crossing the interaction region many times per second (typically one million/s), compensating low density internal gas targets, or low reaction rates in beam-beam collisions. Storage rings are also ideal tools for precise measurements of masses and beta-decay lifetimes of nuclei of relevance for astrophysics. CENTRAL PROBLEMS IN NUCLEAR ASTRO-PHYSICS 1.ScreeningNuclear astrophysics requires the knowledge of the reaction rate R ij between the nuclei species i and j. It is given by R ij = n i n j < σv > /(1 + δ ij ), where σ is the cross section, v is the relative velocity between the reaction partners, n i is the number density of the nuclide i, and <> stands for energy average. Extrapolation procedures are often needed to obtain cross sections at the energy region of astrophysical relevance.While non-resonant cross sections can be rather well extrapolated to the low-energy region, the presence of continuum, or subthreshold resonances, complicate these extrapolations. Another problem is that charged-particle induced reactions are electronscreened in stellar environments [1]. Applying the Debye-Hückel approach, one finds

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“…Note that the values of Q 3b (k) are not interesting in the present context because they are dominated by the factor of −2m e appearing in Eq. (15).…”

Section: The Second Class Of Reaction Involving a Three-body Final Stmentioning

confidence: 99%

“…However, the Q value for beta decay of the fully stripped dysprosium nucleus into a holmium ion with one bound electron is positive, Q ≃ +50 keV. Indeed, this reaction has recently been experimentally observed [15]. The difference in behavior between the neutral atom and the fully stripped nucleus suggests an examination of intermediate, partially stripped ions is needed to identify the most promising candidate reactions for nuclear null tests.…”

Section: Introductionmentioning

confidence: 99%