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Sarriguren P.,CSIC - Institute for the Structure of Matter | Algora A.,University of Valencia | Algora A.,Hungarian Academy of Sciences | Pereira J.,National Superconducting Cyclotron Laboratory | Pereira J.,Joint Institute for Nuclear Astrophysics JINA
Physical Review C - Nuclear Physics

β-decay properties of neutron-rich Zr and Mo isotopes are investigated within a microscopic theoretical approach based on the proton-neutron quasiparticle random-phase approximation. The underlying mean field is described self-consistently from deformed Skyrme Hartree-Fock calculations with pairing correlations. Residual separable particle-hole and particle-particle forces are also included in the formalism. The structural evolution in these isotopic chains including both even and odd isotopes is analyzed in terms of the equilibrium deformed shapes. Gamow-Teller strength distributions, β-decay half-lives, and β-delayed neutron-emission probabilities are studied, stressing their relevance to describe the path of the nucleosynthesis rapid neutron capture process. © 2014 American Physical Society. Source

Crawled News Article
Site: http://www.techtimes.com/rss/sections/science.xml

If you could hold bits of stardust on your palm, what would you do? For physicists at Michigan State University, investigating the particles is the best thing to do. The MSU research team is currently investigating microscopic dust grains from a meteoritic material found on our planet in hopes of unlocking secrets of our galaxy. The particles are believed to be spewed out by stellar explosions that occurred prior to the birth of the sun. The study, which will focus on whether these stardust particles came from classical nova explosions or not, is performed inside the university's National Superconducting Cyclotron Laboratory (NSCL). A classical nova is a thermonuclear explosion on the surface of a small star that is part of two stars orbiting each other, or what is called a binary star system. The explosion would have spewed out stellar material in the form of dust and gas into the space between stars in the galaxy. Some of the dust and gas would have been essential in the creation of our own solar system. Christopher Wrede, spokesperson for the study and an assistant professor of physics at MSU, noted a cosmic recycling process at work in the phenomenon. When stars die, they eject dust and gas that often get recycled into the next generation of planets and stars, he said. He and his colleagues at the NSCL conducted an experiment wherein they created and studied the exotic radioactive nuclei that have the strongest influence on the production of silicon isotopes in a series of novae. The team found that the pre-solar grains contain strange amounts of isotope silicon-30 - an isotope that is quite rare on Earth. Scientists know that silicon-30 is created in a classical novae, but do not know enough yet about the nuclear reaction rates in the explosion to be certain how much silicon-30 was created. This makes the origins of the pre-solar grains uncertain. Still, the new nuclear path and computer models of the explosion will help researchers identify the grains. Typical ways to study classical novae is by using telescopes and looking at the light, but Wrede said the pre-solar grains allow them to study the phenomena in a novel way. "[I]f you can actually hold a piece of the star in your hand and study it in detail, that opens a whole new window on these types of stellar explosions," Wrede said. The initial findings are featured in the journal Physical Review Letters.

Schwarz S.,National Superconducting Cyclotron Laboratory | Bollen G.,Facility for Rare Isotope Beams | Ringle R.,National Superconducting Cyclotron Laboratory | Savory J.,U.S. National Institute of Standards and Technology | Schury P.,University of Tsukuba
Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment

This paper presents a detailed description of the ion cooler and buncher, installed at the Low Energy Beam and Ion Trap Facility (LEBIT) at the National Superconducting Cyclotron Laboratory (NSCL). NSCL uses gas stopping to provide rare isotopes from projectile fragmentation for its low-energy physics program and to the re-accelerator ReA. The LEBIT ion buncher converts the continuous rare-isotope beam, delivered from the gas stopping cell, into short, low-emittance ion pulses, required for high-precision mass measurements with a 9.4 T Penning trap mass spectrometer. Operation at cryogenic temperatures, a simplified electrode structure and dedicated rugged electronics contribute to the high performance and reliability of the device, which have been essential to the successful LEBIT physics program since 2005. © 2016 Elsevier B.V. Source

Thoennessen M.,National Superconducting Cyclotron Laboratory
Nuclear Physics A

The Facility for Rare Isotope Beams (FRIB) will be a new National User Facility for nuclear science, funded by the Department of Energy (DOE), Office of Nuclear Physics (NP) and operated by Michigan State University (MSU). FRIB will cost approximately $550 million to establish and take about a decade to design and build. © 2010 Elsevier B.V. All rights reserved. Source

Lincoln D.L.,Michigan State University | Lincoln D.L.,National Superconducting Cyclotron Laboratory | Holt J.D.,University of Tennessee at Knoxville | Holt J.D.,Oak Ridge National Laboratory | And 14 more authors.
Physical Review Letters

In anticipation of results from current and future double-β decay studies, we report a measurement resulting in a Se82 double-β decay Q value of 2997.9(3) keV, an order of magnitude more precise than the currently accepted value. We also present preliminary results of a calculation of the Se82 neutrinoless double-β decay nuclear matrix element that corrects in part for the small size of the shell model single-particle space. The results of this work are important for designing next generation double-β decay experiments and for the theoretical interpretations of their observations. © 2013 American Physical Society. Source

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