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Kratz, K. L.; Pfeiffer, B.; Thielemann, Friedrich‐Karl; Walters, W. B.

doi:10.1023/a:1012694723985

Cited by 71 publications

(47 citation statements)

References 88 publications

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“…While properties of lighter r-process nuclei have been determined in the laboratory (Kratz et al 2000;Pfeiffer et al 2001;Moller et al 2003), much of the r-process path is through shortlived, very neutron-rich nuclei that are difficult to produce. Future facilities (e.g., the Facility for Rare Isotope Beams [FRIB]) will allow more extensive measurements of relevant masses and β-decay rates.…”

Section: Reconnection In Starsmentioning

confidence: 99%

The impact of recent advances in laboratory astrophysics on our understanding of the cosmos

et al. 2012

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Abstract. An emerging theme in modern astrophysics is the connection between astronomical observations and the underlying physical phenomena that drive our cosmos. Both the mechanisms responsible for the observed astrophysical phenomena and the tools used to probe such phenomena -the radiation and particle spectra we observe -have their roots in atomic, molecular, condensed matter, plasma, nuclear and particle physics. Chemistry is implicitly included in both molecular and condensed matter physics. This connection is the theme of the present report, which provides a broad, though non-exhaustive, overview of progress in our understanding of the cosmos resulting from recent theoretical and experimental advances in what is commonly called laboratory astrophysics. This work, carried out by a diverse community of laboratory astrophysicists, is increasingly important as astrophysics transitions into an era of precise measurement and high fidelity modeling.

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Section: Reconnection In Starsmentioning

confidence: 99%

The impact of recent advances in laboratory astrophysics on our understanding of the cosmos

et al. 2012

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“…[23,16]), there are two types of nuclear structure information that may help to solve r-process problems. First, there is the quite obvious need for nuclear masses, halflives and P n -values of "waiting-point" isotopes located in the r-process boulevard and in particular at magic neutron shells.…”

Section: Experimental Information On R-process Nucleimentioning

confidence: 99%

“…These studies have been benefitting from increasing selectivity in the production, separation and detection of isotopically pure beams using a neutron converter, laser ion sources, isobar separation and multiparameter detector systems (see, e.g. [23,24] ). Presently, experimental masses of only 9 r-process "waiting-point" nuclei (2 at A¥ 80 and 7 at A¥ 132) are known [25].…”

Section: Experimental Information On R-process Nucleimentioning

confidence: 99%

Nuclear Physics Data Relevant to r-Process Nucleosynthesis

Kratz¹,

Ostrowski²,

Pfeiffer³

2005

AIP Conference Proceedings

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Abstract. The production of about half of the heavy elements in nature occurs via the r-process, i.e. a combination of rapid neutron captures, inverse photodisintegrations, and slower β -decays, β -delayed processes as well as fission and possibly interactions with neutrino fluxes. A correct understanding and modelling of this nucleosynthesis process requires the knowledge of nuclear properties far from stability and a detailed description of the astrophysical environments. Experiments at radioactive ion beam facilities have played a pioneering role in exploring the characteristics of nuclear structure in terms of masses and β -decay properties. Initial examinations paid attention to short-lived "waiting-point" nuclei with magic neutron numbers related to the location and height of the solar-system r-process abundance peaks, while more recent activities, mainly in the 132 Sn region, focus on the evolution of shell effects as a function of isospin. In this context, shape transitions and the erosion of the classical shell gaps with possible occurrence of new magic numbers play an important role. Consequences of improved theoretical and experimental nuclear data on calculations of the r-process matter flow will be presented, and the applicability of the long-lived actinides 232 Th and 238 U as cosmo-chronometers will be discussed.

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“…1 shows, that to a large extent the r-process path lies beyond the region of nuclei for which experimental data are available. Exceptions are some nuclei around the N = 50 and N = 82 shell closures, mostly owing to pioneering experiments at ISOLDE (see Pfeiffer et al 2001 [6] and Kratz et al 2000 [7] for recent reviews). Nevertheless, most nuclei in the r-process have been out of reach for experiments so far.…”

Section: The R-processmentioning

confidence: 99%

Nuclear Astrophysics and Nuclei Far From Stability

Schatz

2004

Particles and the Universe

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Unstable nuclei play a critical role in a number of astrophysical scenarios and are important for our understanding of the origin of the elements. Among the most important scenarios are the r-process (Supernovae), Novae, X-ray bursters, and Superbursters. For these astrophysical events I review the open questions, recent developments in astronomy, and how nuclear physics, in particular experiments with radioactive beams, needs to contribute to find the answers. The r-processThe r-process is one of the major nucleosynthesis processes in the universe producing roughly half of all elements heavier than iron. The proposed scenarios for this process include (i) the neutrino-driven wind in core-collapse supernovae [1, 2], (ii) accretion onto and jets from a forming neutron star in core collapse supernovae [3], and (iii) neutron star mergers [4]. So far, all these scenarios have their merits and problems and the question of the site of the r process is essentially open.To address the complex open questions there is clearly a need for more nuclear data such as masses, β decay half-lives, neutron capture rates, fission rates and fission product distributions. For the immediate future r-process calculations will have to rely to a large extent on theoretical predictions. Therefore, experiments are needed not only to provide direct input into r-process calculations, but also to unravel nuclear structure of neutron rich nuclei in general to allow reliable extrapolations beyond the reach of experiments.The nuclei in the r-process path are extremely neutron rich and short lived. Fig. 1 shows, that to a large extent the r-process path lies beyond the region of nuclei for which experimental data are available. Exceptions are some nuclei around the N = 50 and N = 82 shell closures, mostly owing to pioneering experiments at ISOLDE (see Pfeiffer et al. 2001 [6] and Kratz et al. 2000 [7] for recent reviews). Nevertheless, most nuclei in the r-process have been out of reach for experiments so far. To address this problem we have begun to develop an experimental program at the new Coupled Cyclotron Facility at MSU focusing specifically on the weak r-process [8] (see Fig. 1).

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Untitled

Cited by 71 publications

References 88 publications

The impact of recent advances in laboratory astrophysics on our understanding of the cosmos

The impact of recent advances in laboratory astrophysics on our understanding of the cosmos

Nuclear Physics Data Relevant to r-Process Nucleosynthesis

Nuclear Astrophysics and Nuclei Far From Stability

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