Hyperon equation of state for core-collapse simulations based on the variational many-body theory Hajime Togashi Outline
|
|
- Sydney French
- 5 years ago
- Views:
Transcription
1 Hyperon equation of state for core-collapse simulations based on the variational many-body theory Hajime Togashi RIKEN Nishina Center, RIKEN Collaborators: E. Hiyama (RIKEN), M. Takano (Waseda University) 1:Introduction 2:Variational Method for Hyperon Equation of State 3:Application to Compact Stars 4:Summary Outline VA USA, June 28, 2018
2 1: Introduction The era of multi-messenger astronomy has officially begun! The nuclear equation of state (EOS) is important input for numerical simulations. Core-Collapse Supernovae (APJ 786 (2014) 83) Black Hole Formation Figure by K. Nakazato Neutron Star Merger (APJL 789 (2014) L39) 2/14
3 Nuclear EOS for supernova simulations Supernova equation of state (SN-EOS) 3/14 (M. Oertel et al., Rev. Mod. Phys. 89 (2017) ) TNTYST AV18+UIX n, p, α, ( A, Z ) y Togashi et al. (2017)
4 Nuclear EOS for supernova simulations Supernova equation of state (SN-EOS) 3/14 (M. Oertel et al., Rev. Mod. Phys. 89 (2017) ) Skyrme-type effective interaction Relativistic Mean Field Theory TNTYST AV18+UIX n, p, α, ( A, Z ) y Togashi et al. (2017) We have constructed a new SN-EOS with the variational method starting from bare nuclear forces.
5 4/14 Nuclear EOS table with the variational method (HT et al., NPA961 (2017) 78)
6 4/14 Nuclear EOS table with the variational method Uniform EOS: AV18 + UIX (HT et al., NPA961 (2017) 78)
7 4/14 Nuclear EOS table with the variational method Uniform Non-uniform Uniform EOS: AV18 + UIX Non-uniform EOS: Thomas-Fermi method (HT et al., NPA961 (2017) 78)
8 4/14 Nuclear EOS table with the variational method Uniform Non-uniform Uniform EOS: AV18 + UIX Non-uniform EOS: Thomas-Fermi method (HT et al., NPA961 (2017) 78)
9 4/14 Nuclear EOS table with the variational method Uniform Non-uniform Uniform EOS: AV18 + UIX Non-uniform EOS: Thomas-Fermi method We aim to extend the microscopic EOS table to consider Λ hyperon mixing. (HT et al., NPA961 (2017) 78)
10 Nuclear EOS with hyperons HYPERON PUZZLE EOS becomes softer due to hyperon mixing. Maximum mass tends to be lower than the observational data. Hyperon Three-Body Force (ΛNN TBF) D. Lonardoni et al., PRL 114 (2015) SN-EOS with Hyperons Shen EOS with Λ, Σ, Ξ [M max = 1.67 M ] (C. Ishizuka et al., JPG 35 (2008) ) Shen EOS with Λ [M max = 1.75 M ] (H. Shen et al., APJS 197 (2011) 20) LS EOS with Λ [M max = 1.91 M ] (M. Oertel et al., PRC 85 (2012) ) HS EOS with Λ [M max = 2.11 M ] (S. Banik et al., APJS 214 (2014) 22) HS EOS with Λ, Σ, Ξ [M max = 2.04 M ] (M. Marques et al., PRC 96 (2017) ) 5/14
11 Nuclear EOS with hyperons HYPERON PUZZLE EOS becomes softer due to hyperon mixing. Maximum mass tends to be lower than the observational data. Hyperon Three-Body Force Aim of this study (ΛNN TBF) We extend the microscopic EOS table to consider Λ hyperon mixing in a self-consistent manner. SN-EOS with Hyperons D. Lonardoni et al., PRL 114 (2015) Shen EOS We investigate with Λ, Σ, Ξ the [M max effects = 1.67 of Mhyperon ] (C. Ishizuka three-body et al., JPG 35 forces (2008) ) Shen EOS with Λ [M max = 1.75 M ] (H. Shen et al., APJS 197 (2011) 20) (TBF) on the structure of compact stars. LS EOS with Λ [M max = 1.91 M ] (M. Oertel et al., PRC 85 (2012) ) HS EOS with Λ [M max = 2.11 M ] (S. Banik et al., APJS 214 (2014) 22) HS EOS with Λ, Σ, Ξ [M max = 2.04 M ] (M. Marques et al., PRC 96 (2017) ) 5/14
12 2. Variational Method for Hyperon EOS Two-body Hamiltonian ΝN V ij : Argonne v18 (AV18) potential Hyperon Two-Body Central Potentials ΛN V ij : Λ-Nucleon (N) potential (E. Hiyama et al., PRC 74 (2006) ) - Constructed so as to reproduce the experimental binding energies of light Λ hypernuclei with the Gaussian expansion method. ΛΛ V ij : Λ-Λ potential - the experimental double-λ binding energy from 6 He (NAGARA event) ΛΛ (E. Hiyama et al., PRC 66 (2002) ) E 2 : Expectation value of H 2 in the two-body cluster approximation 6/14
13 Expectation value of the Hamiltonian 7/14 Jastrow wave function Φ F : The Fermi-gas wave function Correlation function: p: parity s: two-particle total spin µ: particle pair Cluster-expansion E 2 is the expectation value of H 2 in the two-body cluster approximation with the Jastrow wave function.
14 Nuclear EOS (previous study) Three-Body Energy Modified expectation value of H 3 with Φ F Correction term Repulsive part of UIX pot. is extended to the potential for Hyperon TBF (µ = NNN, ΛNN, ΛΛN, ΛΛΛ) µ P ijk : Three-particle projection operator α NNN : we use the value in the nuclear EOS (Saturation properties+ Thomas-Fermi calculation for atomic nuclei) α ΛNN, α ΛΛN, α ΛΛΛ : We assume 0 α µ α NNN E 3 is the expectation value with the Fermi-gas wave function. 8/14
15 Free energy for Λ hyperon matter 9/14 Total energy per baryon: E (n B, x p, x Λ ) =E 2 + E 3 Baryon number density : n B = n p + n n + n Λ Particle fraction: x i = n i /n B (i = p, Λ) The prescription by Schmidt and Pandharipande is employed to obtain the free energy at finite temperature.
16 Single particle potential for Λ particle Total energy per baryon: E (n B, x p, x Λ ) = E 2 + E 3 Baryon number density : n B = n p + n n + n Λ Particle fraction: x i = n i /n B (i = p, Λ) n B = 0.16 fm -3 x p = 1/2 x Λ = 0 Chemical potential of Λ: µ Λ Energy levels of the Λ single-particle major shells (Rev. Mod. Phys. 88 (2016) ) -32 MeV µ Λ -28 MeV α ΛNN /α NNN /14
17 3. Application to Compact Stars 11/14 Nuclear Matter w/o Hyperon 3BF w/o Hyp. 3BF
18 3. Application to Compact Stars 12/14 µ Λ = -30 MeV (α ΛNN = α NNN ) 0 α ΛΛN = α ΛΛΛ α NNN Nuclear Matter w/o Hyperon 3BF
19 13/14 Supernova matter Application to Supernova matter - Charge neutral and Isentropic matter (The entropy per baryon S ~ 1-2) - Neutrino-free β-stable matter (0 α ΛΛN = α ΛΛΛ α NNN )
20 Summary We construct the EOS for nuclear matter including Λ hyperons at zero and finite temperatures by the variational method. Variational method for hyperon matter The obtained thermodynamic quantities are reasonable. Application of the EOS to compact stars ΛNN three-body force: affects on the single-particle potential and the onset density of Λ hyperon mixing ΛΛN and ΛΛΛ three-body force: affects on the maximum mass of neutron stars (Important for HYPERON PUZZLE!?) The effect of Λ hyperons on neutrino-free matter becomes larger at higher entropies. The era of multi-messenger astronomy has officially begun. It is necessary to construct the reliable EOS for numerical simulations of astrophysical compact phenomena! 14/14
Nuclear equation of state with realistic nuclear forces
Nuclear equation of state with realistic nuclear forces Hajime Togashi (RIKEN) Collaborators: M. Takano, K. Nakazato, Y. Takehara, S. Yamamuro, K. Sumiyoshi, H. Suzuki, E. Hiyama 1:Introduction Outline
More informationNuclear Equation of State for High Density Matter. Matthias Hempel, Basel University NuPECC meeting Basel,
Nuclear Equation of State for High Density Matter, Basel University NuPECC meeting Basel, 12.06.2015 Equation of State for Compact Stars neutron stars core-collapse supernova explosions MH Liebendörfer
More informationThe Nuclear Equation of State
The Nuclear Equation of State Abhishek Mukherjee University of Illinois at Urbana-Champaign Work done with : Vijay Pandharipande, Gordon Baym, Geoff Ravenhall, Jaime Morales and Bob Wiringa National Nuclear
More informationQuantum Monte Carlo calculations of medium mass nuclei
Quantum Monte Carlo calculations of medium mass nuclei Diego Lonardoni FRIB Theory Fellow In collaboration with: J. Carlson, LANL S. Gandolfi, LANL X. Wang, Huzhou University, China A. Lovato, ANL & UniTN
More informationThe EOS of neutron matter, and the effect of Λ hyperons to neutron star structure
The EOS of neutron matter, and the effect of Λ hyperons to neutron star structure Stefano Gandolfi Los Alamos National Laboratory (LANL) Nuclear Structure and Reactions: Weak, Strange and Exotic International
More informationNuclear structure IV: Nuclear physics and Neutron stars
Nuclear structure IV: Nuclear physics and Neutron stars Stefano Gandolfi Los Alamos National Laboratory (LANL) National Nuclear Physics Summer School Massachusetts Institute of Technology (MIT) July 18-29,
More informationThe EOS of neutron matter, and the effect of Λ hyperons to neutron star structure
The EOS of neutron matter, and the effect of Λ hyperons to neutron star structure Stefano Gandolfi Los Alamos National Laboratory (LANL) 12th International Conference on Hypernuclear and Strange Particle
More informationBaryon-Baryon interaction and neutron-star EOS. Y. Yamamoto
2017/3/14 SNP2017 Baryon-Baryon interaction and neutron-star EOS Y. Yamamoto RIKEN Nishina center RMF ours Lagrangian in Baryon-Meson system R F Fitting for saturation parameters Ad hoc parameters to stiffen
More informationProgress of supernova simulations with the Shen equation of state
Progress of supernova simulations with the Shen equation of state Nuclei K. Sumi yoshi Supernovae Numazu College of Technology & Theory Center, KEK, Japan Crab nebula hubblesite.org Applications of nuclear
More informationStrange nuclear matter in core-collapse supernovae
Strange nuclear matter in core-collapse supernovae I. Sagert Michigan State University, East Lansing, Michigan, USA EMMI Workshop on Dense Baryonic Matter in the Cosmos and the Laboratory Tuebingen, Germany
More informationThe EOS of neutron matter and the effect of Λ hyperons to neutron star structure
The EOS of neutron matter and the effect of Λ hyperons to neutron star structure Stefano Gandolfi Los Alamos National Laboratory (LANL) 54th International Winter Meeting on Nuclear Physics Bormio, Italy,
More informationSelf-Consistent Equation of State for Hot Dense Matter: A Work in Progress
Self-Consistent Equation of State for Hot Dense Matter: A Work in Progress W.G.Newton 1, J.R.Stone 1,2 1 University of Oxford, UK 2 Physics Division, ORNL, Oak Ridge, TN Outline Aim Self-consistent EOS
More informationMicroscopic calculation of the neutrino mean free path inside hot neutron matter Isaac Vidaña CFisUC, University of Coimbra
Microscopic calculation of the neutrino mean free path inside hot neutron matter Isaac Vidaña CFisUC, University of Coimbra Landau Fermi liquid theory in nuclear & many-body theory May 22 nd 26 th 2017,
More informationE. Fermi: Notes on Thermodynamics and Statistics (1953))
E. Fermi: Notes on Thermodynamics and Statistics (1953)) Neutron stars below the surface Surface is liquid. Expect primarily 56 Fe with some 4 He T» 10 7 K ' 1 KeV >> T melting ( 56 Fe) Ionization: r Thomas-Fermi
More informationAn EOS implementation for astrophyisical simulations
Introduction Formalism Neutron Stars CCSN An EOS implementation for astrophyisical simulations A S Schneider 1, L F Roberts 2, C D Ott 1 1 TAPIR, Caltech, Pasadena, CA 2 NSCL, MSU, East Lansing, MI East
More informationThe Complete APR Equation of State
The Complete Equation of State C. Constantinou IKP, FZ Jülich 4 May 6, Athens JINA-CEE International Symposium on Neutron Stars in Multi-Messenger Era: Prospects and Challenges Collaborators: B. Muccioli,
More informationHigh density EoS for (core-collapse) supernovae and neutron stars
High density EoS for (core-collapse) supernovae and neutron stars Micaela Oertel micaela.oertel@obspm.fr Laboratoire Univers et Théories (LUTH) CNRS / Observatoire de Paris/ Université Paris Diderot Trento
More informationDense Matter and Neutrinos. J. Carlson - LANL
Dense Matter and Neutrinos J. Carlson - LANL Neutron Stars and QCD phase diagram Nuclear Interactions Quantum Monte Carlo Low-Density Equation of State High-Density Equation of State Neutron Star Matter
More informationb - stable matter of protoneutron star
Mean-field study of the hot b - stable matter of protoneutron star Dao Tien Khoa INST Hanoi, VINATOM EOS of hot nuclear matter with a high neutron-proton asymmetry. EOS of hot b - stable baryon-lepton
More informationDense Matter EoS and applications in Core Collapse SuperNovae and Neutron Stars. Francesca Gulminelli - LPC Caen, France
Dense Matter EoS and applications in Core Collapse SuperNovae and Neutron Stars Francesca Gulminelli - LPC Caen, France Lecture II: nuclear physics in the neutron star crust and observational consequences
More informationNuclear equation of state for supernovae and neutron stars
Nuclear equation of state for supernovae and neutron stars H. Shen Nankai University, Tianjin, China 申虹 In collaboration with 南開大学 天津 H. Toki RCNP, Osaka University, Japan 中国 K. Sumiyoshi Numazu College
More informationInternational workshop Strangeness Nuclear Physics 2017 March, 12th-14th, 2017, Osaka Electro-Communication University, Japan. quark mean field theory
International workshop Strangeness Nuclear Physics 2017 March, 12th-14th, 2017, Osaka Electro-Communication University, Japan The strangeness quark mean field theory Jinniu Hu School of Physics, Nankai
More informationQuantum Monte Carlo calculations of neutron and nuclear matter
Quantum Monte Carlo calculations of neutron and nuclear matter Stefano Gandolfi Los Alamos National Laboratory (LANL) Advances and perspectives in computational nuclear physics, Hilton Waikoloa Village,
More informationSymmetry Energy within the Brueckner-Hartree-Fock approximation
Symmetry Energy within the Brueckner-Hartree-Fock approximation Isaac Vidaña CFC, University of Coimbra International Symposium on Nuclear Symmetry Energy Smith College, Northampton ( Massachusetts) June
More informationNeutrino Mean Free Path in Neutron Stars
1 Neutrino Mean Free Path in Neutron Stars U. Lombardo a, Caiwan Shen a,n.vangiai b,w.zuo c a INFN-LNS,via S.Sofia 44 95129 Catania, Italy b Institut de Physique Nucléaire,F-91406, Orsay France c Institute
More informationNuclear structure III: Nuclear and neutron matter. National Nuclear Physics Summer School Massachusetts Institute of Technology (MIT) July 18-29, 2016
Nuclear structure III: Nuclear and neutron matter Stefano Gandolfi Los Alamos National Laboratory (LANL) National Nuclear Physics Summer School Massachusetts Institute of Technology (MIT) July 18-29, 2016
More informationTowards lattice QCD baryon forces at the physical point: First results
Towards lattice QCD baryon forces at the physical point: First results Takumi Doi (Nishina Center, RIKEN) for HAL QCD Collaboration 2015/09/08 HYP 2015 @ Tohoku U. 1 Nuclear- and Astro- physics based on
More informationNuclear Matter Incompressibility and Giant Monopole Resonances
Nuclear Matter Incompressibility and Giant Monopole Resonances C.A. Bertulani Department of Physics and Astronomy Texas A&M University-Commerce Collaborator: Paolo Avogadro 27th Texas Symposium on Relativistic
More informationCurrent Status of Equation of State in Nuclear Matter and Neutron Stars
Open Issues in Understanding Core Collapse Supernovae June 22-24, 2004 Current Status of Equation of State in Nuclear Matter and Neutron Stars J.R.Stone 1,2, J.C. Miller 1,3 and W.G.Newton 1 1 Oxford University,
More informationSuperfluid Gap in Neutron Matter from a Microscopic Effective Interaction
Superfluid Gap in Neutron Matter from a Microscopic Effective Interaction Omar Benhar INFN and Department of Physics, Sapienza University I-00185 Roma, Italy Based on work done in collaboration with Giulia
More informationRelativistic EOS for Supernova Simulations
Relativistic EOS for Supernova Simulations H. Shen Nankai University, Tianjin, China 申虹 In collaboration with H. Toki RCNP, Osaka University, Japan K. Sumiyoshi Numazu College of Technology, Japan K. Oyamatsu
More informationNuclear equation of state for supernovae and neutron stars
Nuclear equation of state for supernovae and neutron stars H. Shen 申虹 In collaboration with Nankai University, Tianjin, China 南開大学 天津 中国 H. Toki RCNP, Osaka University, Japan K. Sumiyoshi Numazu College
More informationFew Body Methods in Nuclear Physics - Lecture I
Few Body Methods in Nuclear Physics - Lecture I Nir Barnea The Hebrew University, Jerusalem, Israel Sept. 2010 Course Outline 1 Introduction - Few-Body Nuclear Physics 2 Gaussian Expansion - The Stochastic
More informationEquation of state for supernovae and neutron stars
Equation of state for supernovae and neutron stars H. Shen Nankai University, Tianjin, China 申虹南開大学天津中国 In collaboration with H. Toki RCNP, Osaka University, Japan K. Sumiyoshi Numazu College of Technology,
More informationNuclear Structure for the Crust of Neutron Stars
Nuclear Structure for the Crust of Neutron Stars Peter Gögelein with Prof. H. Müther Institut for Theoretical Physics University of Tübingen, Germany September 11th, 2007 Outline Neutron Stars Pasta in
More informationPresent status of modeling the supernova EOS. Matthias Hempel, Basel University Numazu Workshop,
Present status of modeling the supernova EOS, Basel University Numazu Workshop, 1.09.2015 The general purpose supernova EOS neutron stars core-collapse supernovae MH Liebendörfer Crab nebula, Hubble Space
More informationToward a unified description of equilibrium and dynamics of neutron star matter
Toward a unified description of equilibrium and dynamics of neutron star matter Omar Benhar INFN and Department of Physics Sapienza Università di Roma I-00185 Roma, Italy Based on work done in collaboration
More informationNeutron Star Core Equations of State and the Maximum Neutron Star Mass
PORTILLO 1 Neutron Star Core Equations of State and the Maximum Neutron Star Mass Stephen K N PORTILLO Introduction Neutron stars are the compact remnants of massive stars after they undergo core collapse.
More informationAFDMC Method for Nuclear Physics and Nuclear Astrophysics
AFDMC Method for Nuclear Physics and Nuclear Astrophysics Thanks to INFN and to F. Pederiva (Trento) Outline Motivations: NN scattering data few body theory. Few-body many body experiments/observations?
More informationPoS(NIC XII)250. A new equation of state with abundances of all nuclei in core collapse simulations of massive stars
A new equation of state with abundances of all nuclei in core collapse simulations of massive stars 1, Kohsuke Sumiyoshi 2, Shoichi Yamada 1,3, Hideyuki Suzuki 4 1 Department of Science and Engineering,
More informationNuclear electric dipole moment in the Gaussian expansion method
Nuclear electric dipole moment in the Gaussian expansion method Nodoka Yamanaka (ithes Group, RIKEN) In collaboration with E. Hiyama (RIKEN), T. Yamada (Kanto-Gakuin Univ.), Y. Funaki (RIKEN) 2015/10/12
More informationGENERALIZED DENSITY FUNCTIONAL EQUATION OF STATE FOR SUPERNOVA & NEUTRON STAR SIMULATIONS MacKenzie Warren J.P. Olson, M. Meixner, & G.
GENERALIZED DENSITY FUNCTIONAL EQUATION OF STATE FOR SUPERNOVA & NEUTRON STAR SIMULATIONS MacKenzie Warren J.P. Olson, M. Meixner, & G. Mathews Symposium on Neutron Stars in the Multimessenger Era Ohio
More informationHyperonic lattice QCD potentials and hypernuclear few-body problems
Hyperonic lattice QCD potentials and hypernuclear few-body problems H. Nemura, for HAL QCD Collaboration S. Aoki2, T. Doi3, F. Etminan, S. Gongyo2, T. Hatsuda3, Y. Ikeda3, T. Inoue4, T. Iritani2, N. Ishii5,
More informationConstraints from the GW merger event on the nuclear matter EoS
COST Action CA16214 Constraints from the GW170817 merger event on the nuclear matter EoS Fiorella Burgio INFN Sezione di Catania CRIS18, Portopalo di Capo Passero, June 18-22, 2018 1 Schematic view of
More informationNeutron Matter: EOS, Spin and Density Response
Neutron Matter: EOS, Spin and Density Response LANL : A. Gezerlis, M. Dupuis, S. Reddy, J. Carlson ANL: S. Pieper, R.B. Wiringa How can microscopic theories constrain mean-field theories and properties
More informationA Monte Carlo approach to the study of medium-light hypernuclei properties
A Monte Carlo approach to the study of medium-light hypernuclei properties Diego Lonardoni University of Trento - Physics Department INFN - Gruppo Collegato di Trento December 16, 2011 Outline 1. The method
More informationMedium polarization effects and pairing interaction in finite nuclei
Medium polarization effects and pairing interaction in finite nuclei S. Baroni, P.F. Bortignon, R.A. Broglia, G. Colo, E. Vigezzi Milano University and INFN F. Barranco Sevilla University Commonly used
More informationThree-nucleon forces and neutron-rich nuclei
Three-nucleon forces and neutron-rich nuclei Achim Schwenk Facets of Strong Interaction Physics Hirschegg 40 + Bengt 60, Jan. 18, 2012 Happy Birthday Bengt! Outline Understanding three-nucleon forces Three-body
More informationDense QCD and Compact Stars
Dense QCD and Compact Stars ~1 [fm] nucleus ~10 [fm] Neutron star ~10 [km] KEK Workshop (Jan. 21, 2014) Tetsuo Hatsuda (RIKEN) Plan of this Talk 1. QCD Phase Structure 2. Neutron Star and Dense EOS 3.
More informationFour-, Five-, and. Double Strangeness
Four-, Five-, and Six-Body Calculations of Double Strangeness s-shell Hypernuclei H. Nemura Institute of Particle and Nuclear Studies, KEK This talk is based on the work S= 2 world nucl-th/0407033 in collaboration
More informationEquation-of-State of Nuclear Matter with Light Clusters
Equation-of-State of Nuclear Matter with Light Clusters rmann Wolter Faculty of Physics, University of Munich, D-878 Garching, Germany E-mail: hermann.wolter@lmu.de The nuclear equation-of-state (EoS)
More informationFew-particle correlations in nuclear systems
Trento, 9. 4. 2014 Few-particle correlations in nuclear systems Gerd Röpke, Rostock Outline Quantum statistical approach to nuclear systems at subsaturation densities, spectral function Correlations and
More informationGravitational waves from proto-neutron star evolution
Gravitational waves from proto-neutron star evolution Giovanni Camelio in collaboration with: Leonardo Gualtieri, Alessandro Lovato, Jose A. Pons, Omar Benhar, Morgane Fortin & Valeria Ferrari PhD student
More informationAb Initio Calculations of Charge Symmetry Breaking in Light Hypernuclei
Ab Initio Calculations of Charge Symmetry Breaking in Light Hypernuclei Daniel Gazda Nuclear Physics Institute Prague, Czech Republic Together with: A. Gal (HU Jerusalem) Outline Introduction Charge symmetry
More informationThree Baryon Interaction in the Quark Cluster Model 3B Interaction from Determinant Interaction of Quarks as an example
Three Baryon Interaction in the Quark Cluster Model 3B Interaction from Determinant Interaction of Quarks as an example Akira Ohnishi, Kouji Kashiwa, Kenji Morita YITP, Kyoto U. Seminar at Hokkaido U.,
More informationBaryon Interactions from Lattice QCD with physical masses
Baryon Interactions from Lattice QCD with physical masses Takumi Doi (Nishina Center, RIKEN) for HAL QCD Collaboration 2016/01/17 Reimei Workshop @ J-PARC 1 The journey from Quarks to Universe Leinweber
More informationRole of the Nucleus-Nucleus Potential in Sub-barrier Fusion
Role of the Nucleus-Nucleus Potential in Sub-barrier Fusion Şerban Mişicu NIPNE-HH, Bucharest INT Program INT-13-3 Quantitative Large Amplitude Shape Dynamics: Fission and Heavy Ion Fusion Nuclear Physics
More informationThree-nucleon potentials in nuclear matter. Alessandro Lovato
Three-nucleon potentials in nuclear matter Alessandro Lovato PRC 83, 054003 (2011) arxiv:1109.5489 Outline Ab initio many body method Nuclear Hamiltonian: 2- and 3- body potentials Density dependent potential
More informationTRIUMF. Three-body forces in nucleonic matter. Weakly-Bound Systems in Atomic and Nuclear Physics. Kai Hebeler (TRIUMF) INT, Seattle, March 11, 2010
Three-body forces in nucleonic matter Kai Hebeler (TRIUMF) INT, Seattle, March 11, 21 TRIUMF A. Schwenk, T. Duguet, T. Lesinski, S. Bogner, R. Furnstahl Weakly-Bound Systems in Atomic and Nuclear Physics
More informationRelativistic EOS of Supernova Matter with Hyperons 1
Relativistic EOS of Supernova Matter with Hyperons 1 A. Ohnishi, C. Ishizuka, K. Tsubakihara, H. Maekawa, H. Matsumiya, K. Sumiyoshi and S. Yamada Department of Physics, Faculty of Science Hokkaido University,
More informationClusters in Nuclear Matter
Clusters in Nuclear Matter Excellence Cluster Universe, Technische Universität München GSI Helmholtzzentrum für Schwerionenforschung, Darmstadt in collaboration with Gerd Röpke (Universität Rostock) Thomas
More informationVale. Femtoscopy in pp and pa collisions at TeV energies. Andi Bernie Oton Dimitar.
Femtoscopy in pp and pa collisions at TeV energies Laura Fabbietti, Technische Universität München http://www.denseandstrange.ph.tum.de Vale Andi Bernie Oton Dimitar 1 Outline The Hyperon-Nucleon and Hyperon-Hyperon
More informationTensor-optimized antisymmetrized molecular dynamics (TOAMD) with bare forces for light nuclei
Tensor-optimized antisymmetrized molecular dynamics (TOAMD) with bare forces for light nuclei Takayuki MYO Mengjiao LYU (RCNP) Masahiro ISAKA (RCNP) Hiroshi TOKI (RCNP) Hisashi HORIUCHI (RCNP) Kiyomi IKEDA
More informationTheory for nuclear processes in stars and nucleosynthesis
Theory for nuclear processes in stars and nucleosynthesis Gabriel Martínez Pinedo Nuclear Astrophysics in Germany November 15-16, 2016 Nuclear Astrophysics Virtual Institute Outline 1 Ab-initio description
More informationFunctional Orsay
Functional «Theories» @ Orsay Researchers: M. Grasso, E. Khan, J. Libert, J. Margueron, P. Schuck. Emeritus: N. Van Giai. Post-doc: D. Pena-Arteaga. PhD: J.-P. Ebran, A. Fantina, H. Liang. Advantages of
More informationDiscerning the symmetry energy and neutron star properties from nuclear collective excitations
International Workshop XLV on Gross Properties of Nuclei and Nuclear Excitations Hirschegg, Kleinwalsertal, Austria, January 15-21, 2017 Discerning the symmetry energy and neutron star properties from
More informationExplosive nucleosynthesis of heavy elements:
Explosive nucleosynthesis of heavy elements: an astrophysical and nuclear physics challenge Gabriel Martínez Pinedo NUSPIN 2017 GSI, Darmstadt, June 26-29, 2017 32 30 28 34 36 38 40 42 46 44 48 26 28 60
More informationDense QCD and Compact Stars
Dense QCD and Compact Stars ~1 [fm] nucleus ~10 [fm] Neutron star ~10 [km] NFQCD Symposium (Dec. 1, 2013) Tetsuo Hatsuda (RIKEN) Plan of this Talk 1. QCD Phase Structure 2. Dense Matter and Neutron Star
More informationarxiv: v1 [nucl-th] 7 Apr 2009
Thermodynamic properties of nuclear matter with three-body forces V. Somà, and P. Bożek,, Institute of Nuclear Physics PAN, PL-- Kraków, Poland Institute of Physics, Rzeszów University, PL--99 Rzeszów,
More informationNuclear symmetry energy and Neutron star cooling
Nuclear symmetry energy and Neutron star cooling Yeunhwan Lim 1 1 Daegu University. July 26, 2013 In Collaboration with J.M. Lattimer (SBU), C.H. Hyun (Daegu), C-H Lee (PNU), and T-S Park (SKKU) NuSYM13
More informationLight nuclear systems with an antikaon
Light nuclear systems with an antikaon Part 1, Dense kaonic nuclei Revisit the study of kaonic nuclei with AMD+G-matrix+Phen. K bar N potential KEK Theory Center / IPNS Akinobu Doté Part 2, Lambda(1405)
More informationNeutron-rich matter and neutrino-matter interactions based on chiral effective field theory
Neutron-rich matter and neutrino-matter interactions based on chiral effective field theory Achim Schwenk Astrophysical Transients: Multi-Messenger Probes of Nuclear Physics INT, July 29, 2011 Outline
More informationClusters in Dense Matter and the Equation of State
Clusters in Dense Matter and the Equation of State Excellence Cluster Universe, Technische Universität München GSI Helmholtzzentrum für Schwerionenforschung, Darmstadt in collaboration with Gerd Röpke
More informationEquation of state constraints from modern nuclear interactions and observation
Equation of state constraints from modern nuclear interactions and observation Kai Hebeler Seattle, March 12, 218 First multi-messenger observations of a neutron star merger and its implications for nuclear
More informationOrigin of the Nuclear EOS in Hadronic Physics and QCD. Anthony W. Thomas
Origin of the Nuclear EOS in Hadronic Physics and QCD Anthony W. Thomas XXX Symposium on Nuclear Physics - Cocoyoc: Jan 5 th 2007 Operated by Jefferson Science Associates for the U.S. Department of Energy
More informationSpin-Orbit Interactions in Nuclei and Hypernuclei
Ab-Initio Nuclear Structure Bad Honnef July 29, 2008 Spin-Orbit Interactions in Nuclei and Hypernuclei Wolfram Weise Phenomenology Aspects of Chiral Dynamics and Spin-Orbit Forces Nuclei vs. -Hypernuclei:
More informationTheodoros Gaitanos ECT*,
Spectator & participant decay in HIC Theodoros Gaitanos Introduction Theoretical aspects RBUU, relativistic mean-fields, momentum dependence within RMF Equilibration & temperature determination in HIC
More informationStructure of light hypernuclei in the framework of Fermionic Molecular Dynamics
1 Structure of light hypernuclei in the framework of Fermionic Molecular Dynamics Martin Schäfer, Jiří Mareš Nuclear Physics Institute, Řež, Czech Republic H. Feldmeier, T. Neff GSI Helmholtzzentrum für
More informationTDHF Basic Facts. Advantages. Shortcomings
TDHF Basic Facts Advantages! Fully microscopic, parameter-free description of nuclear collisions! Use same microscopic interaction used in static calculations! Successful in describing low-energy fusion,
More informationSpectrum of the Supernova Relic Neutrino Background
Spectrum of the Supernova Relic Neutrino Background Ken ichiro Nakazato (Tokyo University of Science) Numazu Workshop 2015, Sep. 1, 2015 Outline 1. Introduction Neutrino signal from supernovae Supernova
More informationNeutron star structure explored with a family of unified equations of state of neutron star matter
Neutron star structure explored with a family of unified equations of state of neutron star matter Department of Human Informatics, ichi Shukutoku University, 2-9 Katahira, Nagakute, 48-1197, Japan E-mail:
More informationSmall bits of cold, dense matter
Small bits of cold, dense matter Alessandro Roggero (LANL) with: S.Gandolfi & J.Carlson (LANL), J.Lynn (TUD) and S.Reddy (INT) ArXiv:1712.10236 Nuclear ab initio Theories and Neutrino Physics INT - Seattle
More informationConstraining the symmetry energy based on relativistic point coupling interactions and excitations in finite nuclei
7 th International Symposium on Nuclear Symmetry Energy, GANIL (France) 4-7.9.2017 Constraining the symmetry energy based on relativistic point coupling interactions and excitations in finite nuclei N.
More informationHybridization of tensor-optimized and high-momentum antisymmetrized molecular dynamics for light nuclei with bare interaction
Prog. Theor. Exp. Phys. 2015, 00000 (10 pages) DOI: 10.1093/ptep/0000000000 Hybridization of tensor-optimized and high-momentum antisymmetrized molecular dynamics for light nuclei with bare interaction
More informationCluster-gas-like states and monopole excitations. T. Yamada
Cluster-gas-like states and monopole excitations T. Yamada Cluster-gas-like states and monopole excitations Isoscalar monopole excitations in light nuclei Cluster-gas-likes states: C, 16 O, 11 B, 13 C
More informationHeavy-ion reactions and the Nuclear Equation of State
Heavy-ion reactions and the Nuclear Equation of State S. J. Yennello Texas A&M University D. Shetty, G. Souliotis, S. Soisson, Chen, M. Veselsky, A. Keksis, E. Bell, M. Jandel Studying Nuclear Equation
More informationNuclear structure from chiral-perturbation-theory two- plus three-nucleon interactions
Nuclear structure from chiral-perturbation-theory two- plus three-nucleon interactions Petr Navratil Lawrence Livermore National Laboratory* Collaborators: W. E. Ormand (LLNL), J. P. Vary (ISU), E. Caurier
More informationThe oxygen anomaly F O
The oxygen anomaly O F The oxygen anomaly - not reproduced without 3N forces O F without 3N forces, NN interactions too attractive many-body theory based on two-nucleon forces: drip-line incorrect at 28
More informationQRPA Calculations of Charge Exchange Reactions and Weak Interaction Rates. N. Paar
Strong, Weak and Electromagnetic Interactions to probe Spin-Isospin Excitations ECT*, Trento, 28 September - 2 October 2009 QRPA Calculations of Charge Exchange Reactions and Weak Interaction Rates N.
More informationNuclear physics input for the r-process
Nuclear physics input for the r-process Gabriel Martínez Pinedo INT Workshop The r-process: status and challenges July 28 - August 1, 2014 Nuclear Astrophysics Virtual Institute Outline 1 Introduction
More informationNN-Correlations in the spin symmetry energy of neutron matter
NN-Correlations in the spin symmetry energy of neutron matter Symmetry energy of nuclear matter Spin symmetry energy of neutron matter. Kinetic and potential energy contributions. A. Rios, I. Vidaña, A.
More informationNuclear structure I: Introduction and nuclear interactions
Nuclear structure I: Introduction and nuclear interactions Stefano Gandolfi Los Alamos National Laboratory (LANL) National Nuclear Physics Summer School Massachusetts Institute of Technology (MIT) July
More informationNobuya Nishimura Keele University, UK
7. Aug. 2014 @INT Studies of r-process nucleosynthesis based on recent hydrodynamical models of NS-NS mergers Nobuya Nishimura Keele University, UK The r-process: observational request - many r-rich Galactic
More informationLattice QCD studies of strangeness S = -2 baryon-baryon interactions
Lattice QCD studies of strangeness S = -2 baryon-baryon interactions Kenji Sasaki (University of Tsukuba) for HAL QCD collaboration HAL (Hadrons to Atomic nuclei from Lattice) QCD Collaboration S. Aoki
More informationCentral density. Consider nuclear charge density. Frois & Papanicolas, Ann. Rev. Nucl. Part. Sci. 37, 133 (1987) QMPT 540
Central density Consider nuclear charge density Frois & Papanicolas, Ann. Rev. Nucl. Part. Sci. 37, 133 (1987) Central density (A/Z* charge density) about the same for nuclei heavier than 16 O, corresponding
More informationPotential Model Approaches to the Equation of State
Potential Model Approaches to the Equation of State C. Constantinou IKP, FZ Jülich Wednesday, December 3, 214 PALS: M. Prakash, B. Muccioli & J.M. Lattimer Workshop on NEOS for Compact Stars and Supernovae
More informationNuclei as Bound States
Nuclei as Bound States Lecture 1: Hamiltonian Robert Roth Overview Lecture 1: Hamiltonian Prelude Nuclear Hamiltonian Matrix Elements Two-Body Problem Correlations & Unitary Transformations Lecture 2:
More informationFew-Body Hypernuclei. - dependence on NN and 3N force - separation energies based on chiral interactions - CSB of four-body hypernuclei
Mitglied der Helmholtz-Gemeinschaft Few-Body Hypernuclei Andreas ogga, Forschungszentrum Jülich Perspectives of high resolution hypernuclear spectroscopy at Jefferson Lab, ewport ews, VA Motivation umerical
More informationProto-neutron star in generalized thermo-statistics
Proto-neutron star in generalized thermo-statistics K. Miyazaki E-mail: miyazakiro@rio.odn.ne.jp Abstract The proto-neutron star (PNS) is investigated for the rst time in the generalized thermo-statistics.
More informationCoherent and incoherent nuclear pion photoproduction
Coherent and incoherent nuclear pion photoproduction Dan Watts, Claire Tarbert University of Edinburgh Crystal Ball and A2 collaboration at MAMI Gordon Conference on photonuclear reactions, August 2008
More information