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Prof. Brian Fields (Departments of Astronomy and of Physics, University of Illinois)19/06/2017, 09:10Explosive scenarios in astrophysics: observations, theory, and experimentsInvited talk% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Prof. Anton Wallner (The Australian National University)19/06/2017, 09:40Explosive scenarios in astrophysics: observations, theory, and experimentsInvited talk% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Prof. Enrique Zas (IGFAE - University of Santiago)19/06/2017, 10:10The overall picture of the highest energy particles produced in the Universe is changing because of measurements made with the Pierre Auger Observatory. Composition studies point towards an unexpected mixed composition of intermediate mass nuclei, more isotropic than anticipated, which is reshaping the future of the field and underlining the priority to understand composition at the...Go to contribution page
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Dr Jenny Feige (Berlin Institute of Technology)19/06/2017, 10:40% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Prof. Gabriel Martínez Pinedo (Technische Universität Darmstadt)19/06/2017, 11:40Invited talkHalf of the elements heavier than iron are produced by the r process under extreme conditions. To identify its site remains one of the major challenges in nuclear astrophysics. Advances in the description of neutrino-matter interactions and its implementation in core-collapse super- nova modelling have lead to the conclusion that supernova explosions only contribute to the production of...Go to contribution page
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Prof. Taka Kajino (NAOJ, The University of Tokyo)19/06/2017, 12:10Taka Kajino, Shota Shibagaki, Yutaka Hirai, Grant J. Mathews The origin of heavy elements heavier than iron like Au and U are still unknown although sixty years have already passed since the benchmark paper B2FH on the origin of elements in the Universe was published in 1957. GW emitters of both binary neutron-star mergers (NSMs) and core-collapse supernovae (SNe) are viable candidates for...Go to contribution page
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Mr Andre Sieverding (Technische Universität Darmstadt)19/06/2017, 12:40% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Prof. Toshio Suzuki (Nihon University)19/06/2017, 13:00Oral% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Stephane Goriely (Universite Libre de Bruxelles)19/06/2017, 14:30Invited talkThe r-process nucleosynthesis and related nuclear challenges S. Goriely Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles, Belgium Contact email: sgoriely@astro.ulb.ac.be The rapid neutron-capture process, or r-process, is known to be of fundamental importance for explaining the origin of approximately half of the A > 60 stable nuclei observed in nature. In...Go to contribution page
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Dr Jesús Casal (ECT*)19/06/2017, 15:00(file)Go to contribution page
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Georgios Perdikakis (Central Michigan University)19/06/2017, 15:20Oral% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Clemens Wolf (Goethe-University Frankfurt)19/06/2017, 15:40OralThe $^{23}$Al(p,$\gamma$)$^{24}$Si stellar reaction rate has a significant impact of the light-curve emitted in X-ray bursts. Theoretical calculation shows that the reaction rate is mainly determined by the properties of direct capture as well as low-lying 2$^{+}$ states and a possible 4$^{+}$ state in $^{24}$Si. Currently, there is little experimental information on the properties of these...Go to contribution page
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Dr Alba Formicola (LNGS)19/06/2017, 16:30Invited talkAccurate knowledge of thermonuclear reaction rates is important in understanding energy generation, neutrino luminosity and nucleosynthesis in stellar interiors. Natural and Cosmic-ray-induced background can seriously limit the determination of reaction cross-sections at relevant energies for astrophysics. In order to improve the signal-to-noise ratio special care in experimental setups...Go to contribution page
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Dr Matej Lipoglavsek (Jozef Stefan Institute, Ljubljana, Slovenia)19/06/2017, 17:00Electron screening enhances nuclear reaction cross sections at low beam energies. This happens in many astrophysical scenarios, e.g. stellar burning or supernova explosions. Unfortunately, the process is still poorly understood. All currently used calculations are based on the very simple assumption that the electrons distributed evenly on a shell decrease the repulsive potential inside the...Go to contribution page
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Dr Annika Lennarz (TRIUMF)19/06/2017, 17:30% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Mr Felix Heim (Institute for Nuclear Physics, University of Cologne)19/06/2017, 17:50Explosive scenarios in astrophysics: observations, theory, and experimentsOralThe $\gamma$ process is assumed to play an important role in the nucleosynthesis of the majority of the p nuclei. Since the network of the $\gamma$ process includes so many different reactions and - mainly unstable - nuclei, cross-section values are predominantly calculated in the scope of the Hauser- Feshbach statistical model. The values heavily depend on the nuclear physics...Go to contribution page
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Francesca Romana Pantaleo (Universita' degli Studi di Bari, Dipartimento Interateneo di Fisica ''M. Merlin'', Bari, IT, INFN Bari,Bari, IT)19/06/2017, 18:10% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Raffaele Buompane (NA)19/06/2017, 18:307Be(p,g)8B still represents one of the major uncertainties on the predicted high energy component of solar neutrino flux and it has also a direct impact on the 7Li abundance after the Big Bang Nucleosynthesis. Previous experiments producing data with useful precision were performed in direct kinematics, using an intense proton beam on a radioactive 7Be target. The complicated target...Go to contribution page
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Dr Emilio Andrea Maugeri (Paul Scherrer Institut)19/06/2017, 18:50Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \begin{document} \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Prof. Moshe Gai (University of Connecticut)20/06/2017, 08:30% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Nicola Colonna (BA)20/06/2017, 09:00Invited talkNeutron-induced cross sections are a key nuclear physics input for the comprehension of stellar nucleosynthesis of heavy elements, as well as for modeling of light element production in Big Bang Nucleosynthesis. In stars, neutron capture reactions are responsible for the production of the majority of elements heavier than Fe, with two processes contributing more or less equally to the overall...Go to contribution page
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Prof. Jolie Cizewski (Rutgers University)20/06/2017, 09:30% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Dr Massimo Barbagallo (INFN sezione di Bari)20/06/2017, 09:50% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Dr Tanja Heftrich (Goethe University Frankfurt)20/06/2017, 10:10% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Dr Seiya Hayakawa (Center for Nuclear Study, University of Tokyo)20/06/2017, 10:30% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Chris Wrede (Michigan State University)20/06/2017, 11:20Explosive scenarios in astrophysics: observations, theory, and experimentsInvited talkNucleosynthesis and energy generation in classical novae and type I x-ray bursts are driven by nuclear reactions. Many of the thermonuclear rates have substantial uncertainties that preclude accurate comparisons between astronomical observations and astrophysical models. A program of beta decay measurements utilizing intense sources of rare isotopes adjacent to the proton drip line has been...Go to contribution page
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Dr Anu Kankainen (University of Jyväskylä)20/06/2017, 11:50Explosive scenarios in astrophysics: observations, theory, and experimentsOral% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Mr Ryan Wilkinson (University of Surrey)20/06/2017, 12:10Explosive scenarios in astrophysics: observations, theory, and experimentsOral% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Dr Nicolas de Séréville (IPN Orsay)20/06/2017, 12:30Explosive scenarios in astrophysics: observations, theory, and experimentsOral% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Alvaro Tolosa Delgado (IFIC (Instituto de Fisica Corpuscular))20/06/2017, 12:50% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Dr Daid Kahl (University of Edinburgh)20/06/2017, 13:10% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset -0.35in \topmargin 0.305in \oddsidemargin...Go to contribution page
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Prof. Sandrine Courtin (IPHC STrasbourg)20/06/2017, 14:30Invited talkFusion reactions play an essential role in understanding the energy production, the nucleosyn- thesis of chemical elements and the evolution of massive stars. Thus, the direct measurement of key fusion reactions at thermonuclear energies is of very high interest. The carbon burning in stars is essentially driven by the 12C+12C fusion reaction. This reaction is known to show prominent...Go to contribution page
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Dr Richard deBoer (University of Notre Dame)20/06/2017, 15:00% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Dr Michael Febbraro (Oak Ridge National Laboratory)20/06/2017, 15:30% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Dr Daniel Bemmerer (Helmholtz-Zentrum Dresden-Rossendorf)20/06/2017, 15:50% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Mr Nicolas Hubbard (University of York and Aarhus University)20/06/2017, 16:10The 23 Na(α,p) 26 Mg reaction has been identified as having a significant impact on the nucleo- synthesis of elements, such as 23 Na [1] and 26 Al [2], in massive stars, and of light isotopes in type-Ia supernovae [3]. We will present new experimental results, as well as a combined reaction rate based on all available data, and an assessment of its astrophysical impact on massive...Go to contribution page
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Dr Hidetoshi Yamaguchi (Center for Nuclear Study, the University of Tokyo)20/06/2017, 16:30% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset -0.35in \topmargin 0.305in \oddsidemargin...Go to contribution page
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Prof. Rebecca Surman (University of Notre Dame)20/06/2017, 17:10Invited talkThe key role played by nuclear masses in rapid neutron capture, or r-process, nucleosynthesis has long been recognized. Masses set the reaction flow path for an r-process in equilibrium and influence the neutron capture rates, beta decay rates, and fission properties that determine the final abundances. Here we describe modern efforts to quantify the uncertainties in r-process abundance...Go to contribution page
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Gabor Kiss (RIKEN Nishina Center)20/06/2017, 17:40About 50% of the isotopes heavier than iron are synthesized in the so-called astrophysical r-process [1]. During the explosion of a type II supernovae or a Neutron star merger exotic isotopes, closed to the drip line are formed via rapid neutron capture reactions [2]. These, very neutron-rich nuclei emit neutrons after the beta-decay when the decay Q-value is larger than the neutron separation...Go to contribution page
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Artemis Spyrou (NSCL/MSU)20/06/2017, 18:10% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Giuseppe Verde (CT)20/06/2017, 18:30Heavy-ion collisions provide unique access to nuclear structure properties away from saturation density and at finite temperatures. Such structure properties are determined by the equation of state (EoS) and the symmetry energy of nuclear matter that can in turn be studied under laboratory controlled conditions. Such conditions are encountered in neutron stars and in core collapse supernovae...Go to contribution page
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Dr Dan Cozma (IFIN-HH)20/06/2017, 18:50Using a quantum molecular dynamics type transport model coupled to a phase-space coalescence algorithm to determine final spectra of intermediate energy heavy-ion collisions it has been shown that the elliptic flow ratios of neutrons-to-protons and neutrons-to-hydrogen probe, on average, different density regimes of the compressed nuclear matter created in such reactions [1]. This fact is used...Go to contribution page
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Ms Gwenaelle Gilardy (University of Notre Dame)20/06/2017, 19:30PosterAt the end of its life, a massive star collapses into a neutron star. The neutrino flux released during the collapse is so significant that the probability of a neutrino interacting with a nucleus is enhanced enough to have an influence on element nucleosynthesis [1]. The origins of light elements, specifically $^{11}B$, is not fully understood. The $\nu$-process has been proposed as a...Go to contribution page
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Rosanna Depalo (P)20/06/2017, 19:30% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Dr Tamás Szücs (MTA Atomki)20/06/2017, 19:30Poster% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Prof. Tatyana Belyaeva (Universidad Autonoma del Estado de Mexico)20/06/2017, 19:30% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Mr Juan Carlos Morales-Rivera (Universidad Autónoma del Estado de México), Prof. Tatyana Belyaeva (Universidad Autonoma del Estado de Mexico)20/06/2017, 19:30% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % \documentclass[11pt]{article} \usepackage{graphicx} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset -0.35in \topmargin 0.305in \oddsidemargin +0.35in \evensidemargin...Go to contribution page
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Diego Vescovi (PG)20/06/2017, 19:30PosterThe nucleosynthesis of 7Li represents one of the most crucial problems in nuclear astrophysics. The 7Li abundances of several atrophysical sites are hard to be reproduced: in particular, the 7Li abundance observed in the solar photosphere appears to be about 100 times lower than in meteorites. Recently, a new model for non-convective mixing mechanism induced by magnetohydrodynamics (MHD) was...Go to contribution page
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Dr Svetlana Chesnevskaya (IFIN-HH (ELI-NP))20/06/2017, 19:30S. Chesnevskaya1, C.Matei1, D.L. Balabanski1, D.M. Filipescu1, D.G. Ghita1, A. Rotaru1, A. State1, Y. Xu1 G.L. Guardo2, M. La Cognata2, D. Lattuada2, C. Spitaleri2 1. ELI-NP/ IFIN-HH, 30 Reactorului Street, 077125 Magurele, Romania 2. INFN, Laboratori Nazionali del Sud, Via Santa Sofia 62, 95123 Catania, Italy Position-sensitive silicon strip detectors represent one of the best...Go to contribution page
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Mr Matthew Williams (University of York / TRIUMF)20/06/2017, 19:30The electromagnetic mass analyser (EMMA) is a new vacuum-mode recoil mass spectrometer located at the ISAC-II facility at TRIUMF, Vancouver, Canada. Assembly of the spectrometer was completed in 2016, and it received first beam in December 2016. The first in-beam test consisted of an 80 MeV 36Ar beam impinged on a 4.46 μm 197Au foil. The initial test proved to be very successful, with the...Go to contribution page
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Dr Tatyana Belyaeva (Universidad Autónoma del Estado de México)20/06/2017, 19:30Poster\thispagestyle{empty} \begin{center} %%% %%% Title goes here. %%% \TITLE{Critial interaction and strong-absorption distances for the $^{7}$Li $+$ $^{58}$Ni system }\\[3mm] %%% %%% Authors and affiliations are next. The presenter should be %%% underlined as shown below. %%% \AUTHORS{P. Amador-Valenzuela$^{1}$, E.F. Aguilera$^1$, E. Martinez-Quiroz$^1$, D. Lizcano$^1$, J.C....Go to contribution page
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Oscar Trippella (PG)20/06/2017, 19:30% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Giovanni Francesco Ciani (GSSI)20/06/2017, 19:30PosterHeaviest nuclei (A > 58) are synthesized by sequential neutron capture reactions. There are two main processes, depending on their time scale compared with the beta decay lifetime: these are the so called slow (s) and rapid (r) processes. Both produce about half of the stable isotopes beyond iron in the Universe [1]. Focusing on the s process, these take place in low mass (1 − 3M⊙) Asymptotic...Go to contribution page
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Prof. J.E. Horvath (IAG-USP, Sao Paulo, Brazil)20/06/2017, 19:30Poster\textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset -0.35in \topmargin 0.305in \oddsidemargin +0.35in \evensidemargin -0.35in %\renewcommand{\rmdefault}{ptm} % to use Times font \long\def\TITLE#1{{\Large{\bf#1}}}\long\def\AUTHORS#1{ #1\\[3mm]} \long\def\AFFILIATION#1#2{$^{#1}\,$ #2\\} \begin{document} {\small \it Nuclear Physics in Astrophysics 8, NPA8:...Go to contribution page
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Ms Laetitia Canete (University of Jyväskylä)20/06/2017, 19:30% Format: LaTeX2e. % % canete.tex % % \documentstyle[11pt]{article} \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset -0.35in \topmargin 0.305in \oddsidemargin +0.35in \evensidemargin -0.35in \long\def\TITLE#1{{\Large{\bf#1}}}\long\def\AUTHORS#1{ #1\\[3mm]} \long\def\AFFILIATION#1#2{$^{#1}\,$ #2\\} \begin{document} {\small \it ...Go to contribution page
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Mr Laszlo Csedreki (INFN LNGS)20/06/2017, 19:30PosterNuclear Physics in Astrophysics 8, NPA8: 18-23 June 2017, Catania, Italy Introduction of the new LUNA experimental setup for high precision measurement of 13C(α,n)16O reaction for astrophysical purposes L. Csedreki1, G. F. Ciani2, I. Kochanek1 for the LUNA collaboration 1 INFN, Laboratori Nazionali del Gran Sasso LNGS, Assergi, Italy 2 Gran Sasso Science Institute, L’Aquila Contact...Go to contribution page
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Mrs Aleksandra Cvetinović (INFN-LNS Catania)20/06/2017, 19:30PosterFor nucleosynthesis calculations precise reaction rates should be known at energies close to the Gamow peak. Accurate measurements of nuclear reactions performed at these energies [1-5] shows an unexpected enhancement of the cross section at the lowest measurable energies that is attributed to the presence of atomic electrons in the target. In order to observe the bare nuclear cross section,...Go to contribution page
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Carmen Altana (LNS)20/06/2017, 19:30PosterThe future availability of high-intensity laser facilities capable of delivering tens of Petawatts of power (e.g. ELI-NP) into small volumes of matter at high repetition rates will give the unique opportunity to investigate nuclear reactions and fundamental interactions under the extreme plasma conditions realized by laser-matter interactions. Nuclear reactions of astrophysical interest are...Go to contribution page
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Mr Stefan Fiebiger (Goethe University Frankfurt)20/06/2017, 19:30% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Ms Magdalena Skurzok (Jagiellonian University)20/06/2017, 19:30PosterSearch for Deeply Bound Kaonic Nuclear States in AMADEUS experiment M. Skurzok1,2, C. Curceanu2, L. Fabbietti3,4, R. del Grande2,5, P. Moskal1, K. Piscicchia2,6, A. Scordo2, D. L. Sirghi2, Oton Vazquez Doce3,4 1 Institute of Physics, Jagiellonian University, 30-059 Krakow, Poland 2 INFN, Laboratori Nazionali di Frascati, 00044 Frascati, Italy 3 Excellence Cluster Origin and...Go to contribution page
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Dr Aliya Nurmukhanbetova (National Laboratory Astana, Nazarbayev University, Astana, 010000,Kazakhstan), Mr Dosbol Nauruzbayev (National Laboratory Astana, Nazarbayev University, Astana, 010000,Kazakhstan)20/06/2017, 19:30Poster% Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset -0.35in \topmargin...Go to contribution page
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Prof. Sandrine Courtin (IPHC Strasbourg)20/06/2017, 19:30PosterThe STELLA (STELlar LAboratory) experimental station for the measurement of sub-barrier light heavy ion fusion cross sections has been commissioned at the Androm\`{e}de accelerator at IPN, Orsay. These measurements can yield both insight into nuclear cluster effects~[1] and the $S$-factors at energies of astrophysical interest. In particular, $^{12}$C+$^{12}$C fusion was identified as a key...Go to contribution page
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Mr Heinrich Wilsenach (TU-Dresden, IKTP)20/06/2017, 19:30% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Dr Ivano Lombardo (Università di Napoli Federico II and INFN - Sez. Napoli)20/06/2017, 19:30PosterThe study of $^{13}$C structure allows to understand the effects of clusterization in light non-self-conjugated nuclei. The possible presence of rotational bands built on molecular states has been suggested in several papers [1,2]. Furthermore, in recent times, some theoretical papers [3,4] predicted the possible existence of states corresponding to the coupling of a valence neutrons to the...Go to contribution page
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Prof. Rene Reifarth (Goethe University Frankfurt)20/06/2017, 19:30PosterIsomers are metastable states of atomic nuclei. Their half-lifes are about 100 to 1000 times longer than those of the excited nuclear states with prompt g-emissions. If the conditions in an application change on the time scale of isomers' half lifes, their abundances have to be tracked explicitly. The high temperatures under stellar conditions enable the population of higher-lying states...Go to contribution page
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Emily Kading (Graduate Student)20/06/2017, 19:30% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Prof. Dimiter Balabanski (ELI-NP/IFIN)21/06/2017, 08:30Invited talkThe mission of the Extreme Light Infrastructure Nuclear Physics (ELI-NP) research infrastruc- ture are nuclear physics studies with high-power lasers and high-brilliance quasi-monochromatic gamma beams [1,2]. The laboratory will become operational as an user facility in 2019. Two high-power lasers will provide laser pulses on target, each of them having three outputs, e.g....Go to contribution page
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Dr Chiara Mazzocchi (University of Warsaw)21/06/2017, 09:00A new methodology to measure cross-sections for thermonuclear reactions that power the stars is being developed at the University of Warsaw. These reactions take place at different energies according to the respective stellar environment. Such energies are well below the Coulomb barrier and the respective cross-sections are incredibly small, often below the experimental reach. There is a lack...Go to contribution page
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Dr Hernan J. Quevedo (University of Texas)21/06/2017, 09:30Invited talkNuclear fusion from the interaction of very high intensity laser pulses and nm-scale deuterium clusters has been studied since 1999 [1]. These van der Waals bonded clusters can be easily produced in the expansion of a gas jet into vacuum. They absorb the laser pulse energy very efficiently (approaching 100% under certain conditions) and the process by which the ions attain high kinetic...Go to contribution page
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84. Measurements Of Stellar And Big-Bang Nucleosynthesis Reactions Using Inertially-Confined PlasmasDr Alex Zylstra (Los Alamos National Laboratory)21/06/2017, 10:00% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Giovanni Luca Guardo (LNS)21/06/2017, 10:20The Extreme Light Infrastructure-Nuclear Physics (ELI-NP) facility, under construction in Magurele near Bucharest in Romania, will provide high-intensity and high-resolution gamma ray beams that can be used to address hotly debated problems in nuclear astrophysics, such as the accurate measurements of the cross sections of the 24Mg( ,)20Ne reaction, that is funda- mental to determine the...Go to contribution page
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Dr Dario Lattuada (LNS)21/06/2017, 10:40Monte Carlo simulation of photonuclear reactions of astrophysical interest with intense gamma sourcesGo to contribution page
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Jeffery Blackmon (Louisiana State University)21/06/2017, 11:20Explosive scenarios in astrophysics: observations, theory, and experimentsInvited talk% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Dr Oliver Kirsebom (Department of Physics and Astronomy, Aarhus University)21/06/2017, 11:50While the C-12(alpha,gamma)O-16 reaction plays a central role in nuclear astrophysics, the cross section is too small at the energies relevant to stellar helium burning to be directly measured in the laboratory. The beta-delayed alpha spectrum of N-16 can be used to constrain the astrophysical S-factor, but with this approach the S-factor becomes strongly correlated with the assumed...Go to contribution page
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Dr François de Oliveira Santos (GANIL)21/06/2017, 12:10The existence of the Hoyle state is crucial for the nucleosynthesis of the chemical elements heavier than lithium. This state has been the subject of many theoretical studies and philosophical discussions (anthropic principle). The existence of this remarkable state could be explained by the Ikeda conjecture [1,2]. The latter can be formulated simply: The coupling to a nearby cluster decay...Go to contribution page
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Ms Ralitsa Ilieva (University of Surrey)21/06/2017, 12:30Explosive scenarios in astrophysics: observations, theory, and experimentsOral% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Ms Ruchi Garg (University of York)21/06/2017, 12:50We present the first clear observation of the 2+ rotational excitation of the Hoyle state in a beta decay experiment. Coincident detection of β-3α particles from the cascade 12N(β)12C(α1)8Be(α2)α3 have been used to obtain β-α1 angular correlation, which then has been used to determine the strength of the 2+ state relative to that of the 0+ in the 9-12 MeV energy region. The experiment has been...Go to contribution page
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Dr Alison Laird (University of York)21/06/2017, 13:10While core collapse supernovae have long captured the attention of physicists and astronomers, surprisingly little is currently known about the nature of the explosion mechanism. This is due to the complexity of the explosion, the large computational requirements for even 2D simulations, and the lack of precise nuclear physics inputs to these models. One of the few methods by which this...Go to contribution page
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Dr MARCO LIMONGI (INAF-OAR)22/06/2017, 08:30Invited talk
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Dr Raphael Hirschi (Keele University)22/06/2017, 09:00After introducing the slow neutron capture process in massive stars, the so-called weak s process, I will present recent theoretical predictions for the weak s process covering a wide range of initial masses and metallicities. I will in particular discuss the strong effects of rotation at low metallicities and how they boost the weak s process. I will then compare the predictions to...Go to contribution page
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Sara Palmerini (PG)22/06/2017, 09:50We present here the application of a model for a mass circulation mechanism in between radia- tive layers and the base of the convective envelope of low mass AGB stars, aimed at studying peculiar aspects of their nucleosynthesis. Until recently the observational evidence that s-process elements from Sr to Pb are produced by stars ascending the second giant branch could not be explained by...Go to contribution page
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Marcello Lattuada (LNS)22/06/2017, 10:30Invited talk
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Silvio Cherubini (LNS)22/06/2017, 10:45Invited talk
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Prof. Marialuisa Aliotta (University of Edinburgh)22/06/2017, 11:00Invited talkAt the time I began my scientific career as a PhD student under Prof Claudio Spitaleri’s supervision, the Trojan Horse Method was still in its infancy. Like with any new-born idea, it took time and effort and passion to plant the early seeds that would eventually develop into a now well-established method in nuclear astrophysics research. In this talk I will offer my own recollection of...Go to contribution page
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Dr Stefan Typel (IKP, Technische Universität Darmstadt)22/06/2017, 11:15Special session on Claudio Spitaleri achievementsInvited talkBreakup reactions were proposed in 1986 by Gerhard Baur as an indirect method to investigate low-energy charged-particle reactions relevant for nuclear astrophysics [1]. This so-called 'Trojan-Horse method' (THM) allows to extract cross sections of two-particle reactions from suitable transfer reactions with three particles in the final state using quasifree scattering conditions. A...Go to contribution page
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Prof. Carlos Bertulani (Texas A&M University-Commerce)22/06/2017, 11:30Special session on Claudio Spitaleri achievementsEPS Invited SpeakerAccurate measurements of nuclear reactions of astrophysical interest within, or close to, the Gamow peak show evidence of an unexpected effect attributed to the presence of atomic electrons in the target. The experiments need to include an effective “screening” potential to explain the enhancement of the cross sections at the lowest measurable energies. Despite various theoretical studies...Go to contribution page
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Dr Tohru Motobayashi (RIKEN Nishina Center)22/06/2017, 11:45Invited talkI start with my experience for the quasi-free process, which is on the 1H(d,2He)n reaction, where 2He denotes a system of two protons in their unbound singlet S state. The data taken at Saturne in late 1980s were analyzed with plane-wave impulse approximation. The tensor analyzing powers and even the absolute magnitudes of the differential cross sections have been successfully explained. That...Go to contribution page
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Maurizio Busso (PG)22/06/2017, 12:00Invited talk
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Dr Livius Trache (IFIN-HH Bucharest)22/06/2017, 12:15Invited talkIn the house of Trojan Horse Method (THM), I will say a few words about "other" indirect methods we use in Nuclear Physics for Astrophysics. In particular those using Rare Ion Beams that can be used to evaluate radiative proton capture reactions. I addition a few words about work done with the Professore we celebrate today. With a proposal, and some results with TECSA, for a simple method to...Go to contribution page
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Dr Vladilen Goldberg (Cyclotron Institute, Texas A&M University, College Station, Texas, USA)22/06/2017, 12:45Invited talkAlpha-cluster structure populated in the resonance reactions induced by rare beams V.Z. Goldberg, G.V. Rogachev Cyclotron Institute, Texas A&M University, College Station, TX 77843, USA The alpha clusterization manifests itself in remarkable and exotic structures in atomic nuclei. In particular, quasi rotational bands of levels with alternative parities and large alpha cluster reduced...Go to contribution page
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Livio Lamia (LNS)22/06/2017, 14:30Invited talkExperimental nuclear astrophysics aims at measuring astrophysically relevant burning reaction cross sections at the corresponding Gamow energy. However, in spite of the improvements for measuring low-energy nuclear reaction cross sections, the Gamow energy region peak often remains far to be fully explored mainly in the case of charged-particles induced reactions. In such cases, both Coulomb...Go to contribution page
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LUIS ARMANDO ACOSTA SANCHEZ (CT)22/06/2017, 15:00It is well known the importance in Astrophysics of the reactions regarding 26Al. This radioisotope is presented for instance, in the stars where there is H, C and Ne fusion at high temperatures; as well it can be found inside meteorites where it can be deposited or to be created in situ [1]. Considering the importance of the 26Al nuclei, in this work are presented the rst results...Go to contribution page
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Dr György Gyürky (Institute for Nuclear Research (Atomki)22/06/2017, 15:30% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Dr Antti Saastamoinen (Cyclotron Insitute, Texas A&M University)22/06/2017, 15:50The thermonuclear runaway in classical novae proceeds through radiative proton capture re- actions (p,γ) involving proton rich sd-shell nuclei close to the dripline. Many of the capture reactions at typical peak nova temperatures of 0.2-0.4 GK are dominated by resonant capture. Therefore, the key parameters in understanding the astrophysical reaction rates are the energies, decay widths and...Go to contribution page
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Dr Faïrouz Hammache (IPN-Orsay)22/06/2017, 16:50% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Dr Neven Soic (Rudjer Boskovic Institute Zagreb Croatia)22/06/2017, 17:20Detailed knowledge on complex spectroscopy of the $^{24}$Mg nucleus at excitation energies between 14 and 19 MeV has large impact on understanding of clustering in nuclei and on carbon - carbon burning, the $^{12}$C+$^{12}$C fusion, in massive stars. The $^{12}$C+$^{12}$C and $^{16}$O+$^{8}$Be cluster structures (threshold energies are 13.9 and 14.1 MeV respectively) become active in this...Go to contribution page
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Sebastiana Maria Puglia (LNS)22/06/2017, 17:50Oral% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Mr Jos Riley (University of York)22/06/2017, 18:10OralClassical novae are the most common astrophysical thermonuclear explosion [1] and are thought to contribute noticeably to the galactic chemical evolution [2,3]. As one of the few environments that can be modeled primarily from experimental nuclear data, observations would provide a direct test for current hydrodynamic codes. 18F produced in the runaway is the strongest 𝛾-ray source [4]...Go to contribution page
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Dr Vaclav Burjan (Nuclear Physics Institute, CAS)22/06/2017, 18:30OralNuclear Physics in Astrophysics 8, NPA8: 18-23 June 2017, Catania, Italy The direct 18O(p; °)19F capture and the ANC method. V. Burjan1, Z. Hons1, V. Kroha1, J. Mr¶azek1, ·S. Pisko·r1, A. M. Mukhamedzhanov2, L. Trache2, R. E. Tribble2, M. La Cognata3, L. Lamia3, G. R. Pizzone3, S. Romano3, C. Spitaleri3 and A. Tumino3;4 1 Nuclear Physics Institute of Czech Academy of Sciences, 250 68...Go to contribution page
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Dr Emanuel Pollacco (CEA - Saclay)23/06/2017, 08:30Please addGo to contribution page
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Dr Konrad Schmidt (National Superconducting Cyclotron Laboratory, East Lansing, MI, USA)23/06/2017, 09:00% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Dr Christoph Langer (University of Frankfurt a. M.)23/06/2017, 09:20Charged-particle reactions, like (p, g) or (a, g), play a crucial role in many different astrophysical scenarios, such as the p process. Their direct measurement is key for nucleosynthesis model predictions, but is typically hampered by very low cross sections and the lack of intense radioactive ion beams. In this contribution, a novel, powerful method will be presented, which aims at...Go to contribution page
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Giuseppe Cardella (CT)23/06/2017, 09:40% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Pierpaolo Figuera (LNS)23/06/2017, 10:00% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Axel Boeltzig (GSSI)23/06/2017, 10:40The reaction 23Na(p,γ)24Mg links the NeNa and MgAl cycles in stellar hydrogen burning. For temperatures up to 100MK, typical for RGB and low and intermediate mass AGB stars, the rate of this reaction is predominantly determined by the non-resonant component of the cross section and possibly by a narrow resonance at E(c.m.)=138keV. An upper limit for the strength of this resonance has been...Go to contribution page
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Dr Daniele Dell'Aquila (Univ. Napoli Federico II and INFN - Napoli, Italy)23/06/2017, 11:00Given as .tex fileGo to contribution page
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Dr Rosanna Depalo (Università degli Studi di Padova and INFN Padova)23/06/2017, 11:20% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Mr Philipp Scholz (Institut für Kernphysik, Universität zu Köln, Cologne, Germany)23/06/2017, 11:40% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Concetta Parascandolo (NA)23/06/2017, 12:00% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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Viviana Mossa (Università degli Studi di Bari and INFN, sezione di Bari)23/06/2017, 12:20Study of the 2H(p,γ)3He reaction in the Big Bang nucleosynthesis energy range at LUNA V. Mossa for the LUNA collaboration Università degli Studi di Bari and INFN, sezione di Bari Contact email: viviana.mossa@ba.infn.it The Big Bang Nucleosynthesis (BBN) describes the production of light nuclides in the first minutes of cosmic time. It started with deuterium accumulation when the...Go to contribution page
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Dr Tamás Szücs (MTA Atomki)23/06/2017, 12:40% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where `name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset ...Go to contribution page
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