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Prof. Masayuki Matsuo (Department of Physics, Niigata University)13/06/2016, 08:50
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Prof. Ken-ichi Oohara (Niigata University)13/06/2016, 09:00Invited LectureThe gravitational-wave signal GW150914 from merging black holes was observed on 14 September 2015 by the Advanced LIGO. It is not only the first detection of gravitational waves predicted by Albert Einstein just a century ago, but also the first observational evidence for the existence of binary black holes and relatively heavy, stellar-mass black holes larger than 25 solar masses. It has...Go to contribution page
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Prof. Nils Paar (University of Zagreb)13/06/2016, 11:00Invited LectureIn this lecture an overview will be given on the relativistic nuclear energy density functional, and its applications in modeling nuclear properties and weak interaction processes involving nuclei of relevance for astrophysics. In the first step, the formalism of the theory framework will be introduced, and the strategies to constrain the functional will be discussed. In the second part the...Go to contribution page
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Dr Shigehiro Nagataki (Astrophysical Big Bang Laboratory)13/06/2016, 16:00Invited LectureMassive Stars explode as supernovae, and very special supernovae explode as gamma-ray bursts. The explosion mechanism of supernovae is "almost" understood now, while the explosion mechanism of gamma-ray bursts is hardly known. In supernovae/gamma-ray bursts, lots of heavy nuclei are produced by explosive nucleosynthesis. Even r-process nucleosynthesis may happen in special supernovae including...Go to contribution page
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Prof. Timothy Beers (University of Notre Dame)14/06/2016, 09:00Invited Lecture[1st Lecture] The very metal-poor (VMP; [Fe/H] < –2.0) and extremely metal-poor (EMP; [Fe/H] < –3.0) stars provide a direct view of Galactic chemical and dynamical evolution; detailed spectroscopic studies of these objects are the best way to identify and distinguish between various scenarios for the enrichment of early star-forming gas clouds soon after the Big Bang. It has been recognized...Go to contribution page
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Dr Petr Navratil (TRIUMF)14/06/2016, 11:00Invited LectureThe description of nuclei starting from the constituent nucleons and the fundamental interactions among them has been a long-standing goal in nuclear physics. In addition to the complex nature of nuclear forces with two-nucleon, three-nucleon and possibly even four-nucleon components, one faces the quantum-mechanical many-nucleon problem governed by an interplay between bound and continuum...Go to contribution page
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Prof. Maya Takechi (Niigata University)14/06/2016, 16:00Invited LectureThe study and measurements on stable nuclei have been extensively performed since the discovery of atomic nucleus in early 20th century. Their physics properties such as mass, life-time, saturation density property, radii, and their stability have been researched and the knowledge obtained in those studies made the basis of understanding about nuclear structures, strong interaction of nucleons...Go to contribution page
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Prof. Kei Kotake (Fukuoka University)15/06/2016, 09:00Invited LectureIn this lecture, we mainly focus on the explosion mechanisms of core-collapse supernovae. After we briefly review the standard scenario, we talk about a recent status of numerical models where three-dimensional general-relativistic hydrodynamics code including both detailed weak interactions and nuclear equations of state is now meeting with sophisticated neutrino transport scheme. We then...Go to contribution page
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Dr Andreea Oprea (Horia Hulubei National Institute for R&D in Physics and Nuclear Engineering (IFIN-HH))15/06/2016, 14:00Short TalkA.Oprea1, T. Glodariu1,2, D. Filipescu1,2, I. Gheorghe1,2, I. Cata-Danil1, N. Florea1, D. Bucurescu1, D.G. Ghita1, N. Marginean1, R. Marginean1, C. Mihai1, A. Negret1, A. Olacel1, S. Pascu1, R. Suvaila1, L. Stroe1, S. Toma1,3 and N.V. Zamfir1 1 Department of Nuclear Physics, Horia Hulubei National Institute for R&D in Physics and Nuclear Engineering (IFIN-HH)Magurele, Romania 2...Go to contribution page
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Mr Tomoyasu Hayakawa (Kyoto University)15/06/2016, 14:10Short TalkGamma Ray Bursts (GRBs) are among the most energetic events in the universe. GRBs are divided by the duration time into long GRBs and short GRBs. A popular model of the central engine of long GRBs involves a hyper accreting black hole (BH), created by a core collapse of a massive star (the collapsar model) [1]. Indeed, supernovae (SNe) have been observed to be associated with some GRBs since...Go to contribution page
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Mr Fang Ni (Univ. of Tsukuba)15/06/2016, 14:20Short TalkNuclei show a variety of collective phenomena. Especially, excited $0^+$ states in even-even nuclei show puzzling properties. Recent experiments reveal anomalous properties of the low-lying $0^+$ states. We presume that the pairing dynamics plays a significant role in these low-lying excited $0^+$ states. For instance, the $0_2^+$ states in $^{152}$Sm and $^{154}$Gd, which were interpreted as...Go to contribution page
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Mr Chris Griffin (University of Edinburgh)15/06/2016, 14:30Short TalkThe origin of the heavy elements is one of the most fundamental open questions in modern astrophysics, with a notable difficulty being the lack of a complete description of the rapid neutron-capture process (r-process) [1]. Two key quantities used in r-process calculations are β-decay half-lives and β-delayed neutron emission probabilities. The half-lives determine the timescale for the flow...Go to contribution page
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Ms Miyu Masuyama (University of Tokyo, Research center for the early universe)15/06/2016, 14:40Short TalkMagnetars are neutron stars with strong magnetic fields(B~10^14-10^15G). The mechanism to make such a strong magnetic field and what kind of supernova generates a magnetar have not been well understood. Recent observations of supernova remnants associated with magnetars indicate that magnetar progenitors are massive stars and the typical explosion energy is 10^51 erg (e.g. Kumar et al., 2014,...Go to contribution page
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Mr Hideki Shimizu (CNS, University of Tokyo)15/06/2016, 14:50Short TalkWe will present an experimental plan to measure proton resonant elastic scattering with a thick target in inverse kinematics with a novel beam of isomeric Al-26 to be produced with CRIB at RIBF of RIKEN Nishina Center. The steady-state galactic abundance of the Al-26 radionuclide provides a unique window to the ongoing nucleosynthesis in the MIlky Way, as its decay along the galactic plane has...Go to contribution page
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Mr Arthur Choplin (Geneva Observatory)15/06/2016, 15:30Short TalkThe CEMP-no stars (Carbon-Enhanced Metal-poor stars with no sign or weak signs for the presence of s- or r-elements) are long-lived small mass stars presenting a very low iron content and overabundances of carbon. Their chemically peculiar abundance pattern could be inherited from a previous massive star (the source star) that has lost mass through winds or at the time of the supernova....Go to contribution page
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Mr Takayuki Miyagi (Department of Physics, the University of Tokyo)15/06/2016, 15:40Short TalkOwing to the recent computational progress, the medium-mass nuclei have been investigated recently by the ab initio methods such as the coupled-cluster method, in-medium similarity renormalization group approach, and self-consistent Green’s function method. Similarly to these methods, the unitary-model-operator approach (UMOA) can also be applied to the medium-mass nuclei. So far, we...Go to contribution page
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Ms Jacqueline Den Hartogh (Keele University)15/06/2016, 15:50Short TalkAfter the central He burning in exhausted, stars with an initial mass of 1.5-3 solar masses start the AGB phase. In this phase, the s-process takes place, which is producing about half of all elements heavier than iron. Our non-rotating AGB stellar models calculated with MESA (see Battino et al., submitted) include a treatment of convective boundary mixing based on the results of hydrodynamic...Go to contribution page
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Cathleen Fry (MSU/NSCL)15/06/2016, 16:00Short TalkIn classical novae, the 30P(p,g)31S reaction potentially acts as a bottleneck in nucleosynthesis flow to higher masses. Knowledge of this reaction rate is necessary for the modeling of elemental and isotopic ratios in classical novae, which affect proposed nova thermometers and presolar grain identification, respectively. While most of the resonance energies are known experimentally, the...Go to contribution page
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Ms Eri Miyata (graduate school of science Niigata University)15/06/2016, 16:10Short TalkIn order to improve the resolution of particle identification for radioactive beams, it is important to develop the high time resolution detector to measure TOF. We have developed the high time resolution TOF detector which detects the Cherenkov light emitted when RI beam passes through the high refractive index radiator. Generally, the plastic scintillation counter has been commonly used as a...Go to contribution page
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Mr Vi Phong (RIKEN Nishina Center)15/06/2016, 16:20Short TalkVi Ho Phong1,2, Shunji Nishimura1, Giuseppe Lorusso3,4, Jorge Agramunt5, Alejandro Algora5, Roger Caballero-Folch6, Francisco Calvino7, Guillem Cortes7, Thomas Davinson8, Iris Dillmann6, Alfredo Estrade9, Robert Grzywacz10, Gabor Kiss1, Keishi Matsui1, Fernando Montes12, Cesar Domingo Pardo5, Albert Riego8, Krzysztof Rykaczewski13, Jose Luis Tain5, Ariel Tarifeno Saldivia7, Alvaro Tolosa5,...Go to contribution page
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Ms Erika Holmbeck (University of Notre Dame)15/06/2016, 16:30Poster PresentationMetal-poor stars in the Galactic halo have been studied for the past half century in order to understand the chemical evolution of the Galaxy, extending back to the first generations of stars born in the Universe. However, only within the last twenty years have very metal-poor, highly r-process-element-enhanced (r-II) stars begun to shed light on the cosmic origin of the r-process elements....Go to contribution page
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Mr Taygun Bulmus (Mimar Sinan FA University)15/06/2016, 16:30Poster PresentationThe neutrinos that emerge in the core collapse supernovas play an important role in the cooling mechanism of the proto-neutron star (PNS). The luminosity of the neutrinos that emerge in the explosion is estimated to be 10^{52} erg/s [1]. Although the neutrinos’ interaction cross-section is relatively very small, such a dense medium makes it possible for the neutrinos to engage in...Go to contribution page
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Mr Ryo IWAMI (Niigata University)15/06/2016, 16:30Poster PresentationWe study scaling behavior of a chiral order parameter in the low density region, performing a simulation of two-flavor lattice QCD with improved Wilson quarks. It have been confirmed that the scaling behavior of the chiral order parameter defined by a Ward-Takahashi identity agrees with the scaling function of the three-dimensional O(4) spin model at zero chemical potential. We discuss the...Go to contribution page
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Mr Felix Heim (Institute for Nuclear Physics, University of Cologne)15/06/2016, 16:30Poster PresentationThe activation technique is a widely used method for the determination of cross- section values for charged-particle induced reactions at astrophysically relevant energies. Since network calculations of nucleosynthesis processes often depend on reaction rates calculated in the scope of the Hauser-Feshbach-statistical model, these cross-sections can be used to improve the nuclear-physics...Go to contribution page
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Mr Kento Inaba (Kyoto University)15/06/2016, 16:30Poster PresentationDifferential cross sections for elastic electron scattering reflect on charge distribution of nuclei because they are given by products of the Mott cross section and charge form factors. Charge distribution of nuclei is obtained from the Fourier transform of the charge form factors. We conducted an experiment of electron scattering to study the relations between the cross section and the...Go to contribution page
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Ms Yuna Ogata (Nihon University)15/06/2016, 16:30Poster PresentationWe study neutrino oscillations of reactor neutrinos, anti-electron neutrinos, both in the short- and medium- to long-baseline cases. THe survival and generation probabilities of the neutrinos are calculated within the three-flavor mixing model, and the dependence of the probabilities on the mass hierarchy and CP-phase is investigated. We find that the hierarchy can be determined from the...Go to contribution page
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Ms Momoka Mito (Nihon University)15/06/2016, 16:30Poster PresentationWe study neutrino oscillations of atomospheric neutrinos when they go through the earth, which has a dense core and a mantle with less density. Survival probabilities of atomospheric muon neutrinos are calculated within the three-flavor mixing model. Dependence of the probability at the exit surface of the earth on the neutrino energy and zenith angle is investigated. The survival probability...Go to contribution page
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Mr Masanori Kaneko (Department of Physics, Kyoto University)15/06/2016, 16:30Poster PresentationThe nuclear equation of state (EoS) is one of the most fundamental expressions that describe the basic relationship between energy, pressure, density, temperature, and isospin asymmetry δ=(ρ_n-ρ_p)/(ρ_n+ρ_p) for a nuclear system. For a neutron star, which has extreme asymmetry of its isospin, the symmetry energy term of the EoS is considered to play an important role in determining physical...Go to contribution page
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Mr Kanji Mori (the University of Tokyo)15/06/2016, 16:30Poster PresentationRecent experimental results have confirmed a possible reduction in the GT+ strengths of pf-shell nuclei. These proton-rich nuclei are of relevance in the deflagration and delayed-detonation and explosive burning phases of Type Ia supernovae (SNe Ia). While prior GT strengths result in nucleosynthesis predictions with a higher-than-expected neutron-excess isotopes for the elements...Go to contribution page
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Mr Mizuki SHIROGANE (Niigata University)15/06/2016, 16:30Poster PresentationWe calculate the energy gap (latent heat) and pressure gap between the hot and cold phases of the SU(3) gauge theory at the first order deconfining phase transition point. We perform simulations around the phase transition point with the lattice size in the temporal direction Nt = 6; 8 and 12 and extrapolate the results to the continuum limit. We also investigate the spatial volume...Go to contribution page
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Mr Kazuya Chikaato (graduate school of science Niigata University)15/06/2016, 16:30Poster PresentationWe have studied nuclear reactions for Long-Lived-Fission-Products (LLFP) 90Sr for the purpose of nuclear transmutation. The nuclear data of proton and deuteron beam for LLFP target is one of the essential dataset for the study of transmutation. However, the nuclear data for those LLFP are insufficient and the accumulation of precise nuclear data is required. The interaction cross sections...Go to contribution page
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Ms Azusa Inoue (RCNP)15/06/2016, 16:30Poster PresentationA. Inoue1, A. Tamii1, K. Abe3, S. Adachi1, N. Aoi1, M. Fukuda2, G. Gey1, T. Hashimoto4, S. Hayakawa3, K. Hirakawa1, E. Ideguchi1, K. Matsuta2, M. Mihara2, S. Noji1, T. Shima1, H. Shimizu3, R. Tang1, T. D. Trong1, H. Yamaguchi3, L. Yang3 1 Research Center for Nuclear Physics, Osaka University 2 Department of Physics, Osaka University 3 Center for Nuclear Study, University of Tokyo 4...Go to contribution page
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Mr Maulen Nassurlla (master student)15/06/2016, 16:30Poster PresentationN. Burtebayev 1, J.T. Burtebayeva 1, A. Duisebayev1, T. Zholdybayev1, M. Nassurlla 2, S.B. Sakuta 3, S. Kliczewski4, E. Piasecki4, K. Rusek5, A. Trzcińska5, M. Wolińska-Cichocka5, S.V. Artemov 6 1Institute of Nuclear Physics of National Nuclear Center, Almaty, Kazakhstan; 2Al-Farabi Kazakh National University, Almaty, Kazakhstan; 3National Research Center “Kurchatov Institute”, Moscow,...Go to contribution page
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Mr Matthew Gilmer (North Carolina State University)15/06/2016, 16:30Poster PresentationMatthew Gilmer1, Alexandra Kozyreva2, Raphael Hirschi2, Carla Frohlich1 1 North Carolina State University, Raleigh, NC 27695-8202 2 Astrophysics group, Keele University, Keele, Staffordshire, ST5 5BG, UK The new highly diverse class of supernovae, Super Luminous Supernovae (SLSNe), along with observations of Very Massive Stars (VMS) in the Local Universe have helped to revive interest...Go to contribution page
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Shinkuro Sakai (Niigata University)15/06/2016, 16:30Poster PresentationIn couple of decades, thanks to the development of the radioactive isotope beam technology, the study for neutron-rich light nuclei has become possible. The nuclei in this region often have the exotic properties, such as the neutron halo, disappearance of the canonical magic numbers, and appearance of the new magic numbers. Recently, in the experimental study of the neutron-rich nuclei[1],...Go to contribution page
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Mr Yoshihiko Kobayashi (Niigata University)15/06/2016, 16:30Poster PresentationLow-lying (less than 1 MeV) resonances in neutron-rich nuclei has important role in neutron capture phenomena like the r-process. We focus on a new type resonance in superfluid nuclei. That is called quasi-particle resonance [1,2]. Many nuclei with open-shell configuration have superfluidity generated by pairing correlation. The pairing correlation causes continuum coupling in weakly bound...Go to contribution page
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Rodney Orford (McGill University)15/06/2016, 16:30Poster PresentationThe astrophysical rapid neutron capture process (r process) of nucleosynthesis is thought to be responsible for the production of roughly half of the elements heavier than iron. Despite its large influence in explaining the observed abundance of heavy elements, much of the r process is still poorly understood. A more thorough library of nuclear data, including masses, of neutron-rich nuclei is...Go to contribution page
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Sanjana Sinha (North Carolina State University)15/06/2016, 16:30Poster PresentationCore-collapse supernovae are the extremely energetic deaths of massive stars. As such, they play a vital role in the synthesis and dissemination of many heavy elements in the universe. In the past, core-collapse supernova nucleosynthesis calculations have relied on artificial explosion methods that do not adequately capture the physics of the innermost layers of the star. The PUSH method,...Go to contribution page
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Mr Shihang Shen (RIKEN)15/06/2016, 16:30Poster PresentationNuclear structure information serves as important inputs for the study of nuclear astrophysics, for example, the equation of state for neutron star, and the nuclear masses and decay rates for nucleosynthesis . Nowadays ab initio methods have been paid more and more attention since they study nuclear structure from the realistic nucleon-nucleon (NN) interaction, which can be obtained either...Go to contribution page
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Mr Nicolas Hubbard (University of York)15/06/2016, 16:30Poster PresentationWithin the C/Ne convective shell of a massive star the 23Na(α,p)26Mg reaction is an important source of protons for 26Al production[1]. This shell is also the main source of Na ejected by core-collapse supernovae. A new experimentally determined reaction rate has been calculated across the relevant temperature range based on 3 new cross-section measurements [2-4] and angular distributions...Go to contribution page
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Mr Kenta Yabe (Niigata University)15/06/2016, 16:30Poster PresentationWe study the transverse polarization of hyperons produced in the high-energy unpolarized proton-proton collision in the framework of the collinear factorization. To understand this phenomenon is one of the big challenges in high-energy hadron physics because it can’t occur in the conventional framework for high-energy inclusive reactions: parton model and perturbative QCD. However, using the...Go to contribution page
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Dr Rosario Pizzone (infn lns)16/06/2016, 09:00Invited LectureThe low energy behavior of reactions of astrophysical interest is one of the most important input to calculate the reaction rates of astrophysical importance and therefore to evaluate their impact on astrophysical environments. Astrophysical energy range are so low that only in few cases direct measurements in those energy ranges were possible. This is even truer for reactions induced by...Go to contribution page
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Dr Maria Lugaro (Konkoly Observatory, Hungarian Academy of Sciences)17/06/2016, 09:00Invited LectureAll stars born with mass between roughly 1 and 10 solar masses evolve through the asymptotic giant branch (AGB) phase before disappearing from sight as white dwarfs. On the AGB they synthetise elements in their deep, hot layers, mix them to the surface, and shed them into their surrounding by stellar winds. Through this series of processes(nucleosynthesis, mixing, and winds) AGB stars...Go to contribution page
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Prof. Shinji Ejiri (Niigata University)17/06/2016, 11:00Invited LectureI will talk about the phase transition of quantum chromodynamics (QCD) at high temperature and high density. The color confinement and the chiral symmetry breaking are the most important properties of the strong interaction and these properties vary depending on temperature and density. The numerical simulation of lattice QCD is a powerful tool to study the strong interaction. In this lecture,...Go to contribution page
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Dr Tohru Motobayashi (RIKEN Nishina Center)17/06/2016, 17:30
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