Current Status of Equation of State in Nuclear Matter and Neutron Stars
|
|
- Corey Robbins
- 6 years ago
- Views:
Transcription
1 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, Oxford, UK 2 Physics Division, ORNL, Oak Ridge, TN 3 SISSA, Trieste, Italy
2 Outline 1. General properties of EOS in nuclear matter 2. Classification according to models of N-N interaction 3. Examples of EOS sensitivity to the choice of N-N interaction 4. Consequences for supernova simulations 5. Constraints on EOS 6. High density nuclear matter (HDNM) 7. New developments
3 Equation of State is derived from a known dependence of energy per particle of a system on particle number density: E/ A= E ( n) or F / A= F ( n) I. E ( or Boltzman free energy F = E-TS for system at finite temperature) is constructed in a form of effective energy functional (Hamiltonian, Lagrangian, DFT/EFT functional or an empirical form) II. An equilibrium state of matter is found at each density n by minimization of E (n) or F (n)
4 III. All other related quantities like e.g. pressure P, incompressibility K or entropy s are calculated as derivatives of E or F at equilibrium: Pn ( ) = 2 E ( n) n n sn F ( n) = T ( ) ny, p P n n n Kn ( ) = 9 = 18n + 9n n n n 2 ( ) E ( ) 2 E ( ) 2 IV. Use as input for model simulations
5 (Very) schematic sequence of equilibrium phases of nuclear matter as a function of density: <~2x10-4 fm -3 ~2x10-4 fm -3 ~0.06 fm -3 Nuclei in electron gas Nuclei in Neutron + Electron gas Pasta phase ~0.1 fm fm -3 >0.5 fm -3 n,p,e,µ (β equilibrium) Nucleons + heavy baryons + leptons Quarks???
6 Ground state: Symmetric (SNM) - saturation density n fm-3 n p = n n = 1/2 energy per particle E/A (n 0 ) - 16 MeV symmetry energy a s E/A (SNM) -E/A (PNM) MeV Incompressibility K(n 0 ) MeV Pressure P(n 0 ) 0 Excited states: Asymmetric matter n+p+e+µ (in β-equilibrium) density dependence of : - proton fraction y p = n p /n - symmetry energy S (coefficient a s ) - chemical potentials µ n, µ p, µ e, µ µ Pure neutron (PNM) - does not saturate (E/A > 0)
7 To construct the energy functional we need nuclear and particle physics models: Expectation value of the total energy: E =< φ,( T + V) φ > T kinetic energy, V total potential energy of the system Φ is a Slater determinant of single particle states φ i
8 Theories Relativistic Non-relativistic Potentials Realistic Phenomenological Reid 93 Nijmegen II Argon v18 (A18) } } Local non-rel Skyrme } Gogny Nijmegen I CD Bonn Non-local non-rel Local rel SMO } NL +
9 Realistic bare nucleon (OBE) Hjorth-Jensen, Phys.Rep,261,125(1995) ~20-60 adjustable parameters Several thousand data points Free nucleon-nucleon scattering and properties of deuteron Renormalization needed for use in dense medium Brueckner-Hartree-Fock Dirac-Brueckner-Hartree-Fock Variational methods, etc to calculate G-matrix EOS for SNM and PNM (usually) + Further parameterization needed to obtain inhomogeneous NM Phenomenological density dependence adjustable parameters Several hundred data points Finite nuclei (g.s.) and properties of nuclear matter at saturation density Hartree-Fock, Dirac-Hartree, Dirac-Hartree-Fock etc to calculate selfconsistently equilibrium potential energy EOS for SNM, PNM and inhomogeneous NM
10 Examples Non-relativistic Hartree method - phenomenological Skyrme potential Vautherin and Brink, PRC 5, 626 (1972) V = v + v (2) (3) i, j i, j, k i< j i< j< k 2 p 1 1 E = < i i >+ < ij v ij > + < ijk v ijk > 12 AS 123 i 2m 2 i, j 6 i, j, k AS V 12 (v 123 ) parameterized two (three)-body potential Relativistic Dirac-Brueckner method realistic Bonn potential Li et al., PRC 45, 2782 (1992) 2 2 % + % i 1 % % % mm p m E = + < ij G( z) ij ji> m E% 2 EE % % i k i i, j< k i j f f For notation see the above reference G-matrix
11 Equation of State of Akmal et al. PRC 58, 1804 (1998) thought of as the most complete study to date of HDNM Potentials: A18 (two-body): static, long range one-pion exchange + PHENOMENOLOGICAL medium and short range part dependent on 18 two-body operators UIX (three-body) static, long-range two-pion exchange + PHENOMENOLOGICAL medium range repulsive term + Relativistic boost correction to the two body N-N interaction + Ad hoc density dependent term γ 2 ρ 2 e -γ 3 ρ which provides 25% (~4 MeV) correction to the E/A of symmetric nuclear matter to reach the empirical value 16 MeV For densities <0.1 fm -3 EOS by Lorenz et al., PRL 70,379 (1993) is used.
12 Akmal et al., E/A as a function of baryon number density At saturation density 0.16 fm -3 the expected value of E/A=16 MeV
13 Akmal et al., Sensitivity of density dependence of E/A to the form of a realistic potential Symmetric nuclear matter Pure neutron matter
14 Density dependence of E/A in nuclear matter for phenomenological Skyrme interactions (87 tested) 80 Energy per partlicle [MeV] SkO (I) PNM BEM SNM SkX (II) MSk7 (III) n [fm 3 ] n [fm 3 ] n [fm 3 ] J.R.Stone et al., PRC 68, (2003)
15 FINITE TEMPERATURE LATTIMER-SWESTY EOS Current standard in supernova modelling Nucl.Phys. A535, 331 (1991) and Matter consisting from electrons, positrons, photons, Free nucleons, alpha particles (representing light nuclei) and single species for heavy nuclei. Compressible liquid drop model non-relativistic fermion kinetic energies, schematic two-body density dependent interaction (based on the Skyrme model) schematic model for multi-body interactions
16 Temperature and effective mass: m*/m T S = 1, Y p = 0.3 Lattimer-Swesty: Three nuclear forces represented by K = 180, 220 and 375 MeV with m*/m = 1 Temperature is independent from the nuclear force for densities higher than ~0.1 fm-3, i.e for pure nuclear matter Onsi et al., PRC55,3139 (1997) Fully temperature dependent ETFSI with Skyrme interactions RATP (m*/m=0.67), SkSC6 (m*/m=1) Temperature is dependent on the force in the whole region of densities
17 Lattimer-Swesty: Pressure/baryon as a function of ln n: Significant differences in nuclear matter phase in dependence on the nuclear force. Onsi et al: Pressure as a function of n n[fm -3 ] LS Onsi
18 Adiabatic index: ln Γ= ln P n sy, p Very important in hydrodynamic calculations A measure of stiffness of the matter at phase boundaries Reflects nature and treatment of phase changes Examples I. Akmal et al : transition between normal low density matter (LDP) and high density matter with condensed pions (HDP) II. LS: transition from pasta phase to pure nuclear matter phase ( proton rich nuclei in neutron vapor + α particles, } + e neutron bubbles + α in dense proton rich matter) III. Onsi et al: transition between droplet and bubble phase transition between bubble and homogeneous matter
19 Adiabatic index as calculated by Akmal et al, PRC 58, 1804 (1998) Discontinuity at n~0.2 fm -3 represents a LDP -> HDP transition B - bag constant for quark admixtures
20 Adiabatic index as a function of ln n (LS) and n (Onsi) for s=1 and Y p =0.3 LS Onsi et al. droplet-bubble bubble NM pasta NM Note different x and y-axis scales Values of Γ differ from Akmal et al
21 Bound nuclei in e + n gas beyond Wigner-Seitz model Magierski and Heenen, PRC 65, (2002) Shell effects in inhomogeneous asymmetric nuclear matter lead to a complicated pattern of density dependent phases and phase transitions not taken into account by previous models A STATE-OF-ART TREATMENT OF THE PASTA PHASE
22 "Core-Collapse Supernovae at the Threshold" H.-T. Janka, R. Buras, K. Kifonidis, A. Marek and M. Rampp (Proceedings IAU Coll.~192, Valencia, Spain, April , 2003, Eds. J.M.~Marcaide ad K.W.~Weiler, Springer Verlag) Shen et al, NP A637, 435 (1998) RMF Hillebrant and Wolff, 1985 Skyrme T-dependent Hartree-Fock Shock radius Electron neutrino luminosity
23 Sensitivity of predicted nuclear matter parameters to details of EOS Search for constraints to narrow down the variety of models. Example of an efficient constraint for a non-relativistic Skyrme potential in Hartree-Fock approximation Density dependence of the symmetry energy 1 S ( n) = E ( n, Yp = 0) E ( n, Yp = ) where Yp = 2 or d E 1 p = E p = + 2 p 2 2 dyp 2 E ( ny, ) ( ny, ) ( )( n)( Y ) 1/2 n p n
24 ρ / ρ n/ n o o Bao-An Li, PRL 88, (2002) SNM ground state at all densities δ = n n n n + n n p p δ = 0 symmetric δ = 1 pure neutron PNM ground state at high densities
25 Density dependence of the symmetry energy is the main criterion for distinction between Skyrme parameterizations Group I Group II Group III SkO (I) a s [MeV] SkX (II) 0 25 MSk7 (III) n [fm 3 ] n [fm 3 ] n [fm 3 ] SkO, SkX, MSk7 examples of Skyrme potentials J.R.Stone at al., PRC68, (2003)
26 Gravitational mass versus radius for T=0 non-rotating neutron stars calculated using Skyrme EOS based on parameterizations I, II and III 2 M [M sun ] SLy4(I) SkO(I) SkI3(I) SkI1(I) SIII(II) SkM * (II) SkX(II) Skz4(II) No reasonable neutron stars are produced by Skyrme interactions of group III R [km] R[km]
27 Constraint from maximum mass of a neutron star Nice et al., Pulsar+white dwarf binary Arecibo telescope timing analysis orbital period 0.26 days > M solar with 95% confidence If this observation is confirmed, a large number of EOS would be eliminated Structure of HDM would be questioned as the presence of hyperons and quarks is known to lower the maximum mass of a neutron star.
28 Can hyperons be eliminated from neutron star models? Significant lowering of maximum mass of a cold neutron star by presence of hyperons at high densities However, the classical Bethe-Johnson EOS includes matter with hyperons and still predicts maximum mass ~2 solar masses.
29 No calculation of ground state properties of finite nuclei heavier then C is possible as yet for realistic interactions Calculated neutron skin in 208 Pb for 87 Skyrme models in comparison to experimental data Experimental data on neutron skins from proton scattering are model dependent! Clark et al. PRC 67, (2003) Most precise data (1.5%) from atomic parity violation measurement in electron scattering at JLAB expected in about 2 years Horowicz et al. PRC63, (2001)
30 Heavy Ion Collisions Testing of the density dependence of S Bao-An Li et al., PRL 78, 1644 (1997):88, , (2002) Danielewicz et al, Science 298, 1592 (2002) The only terrestrial situation where HD neutron rich matter can be formed up to several times nuclear saturation density n o (MSU, Darmstadt, RHIC) Observables: π- to π+ ratio neutron-proton collective flow transverse and elliptical flow of particles from high density regions during collisions
31 Microstructure of NS at High Densities : Ted Barnes talk tomorrow Most models predict presence of hyperons and quarks; some include boson condensates of pions and kaons. The general problem is that calculation of thresholds (chemical potentials) for these particles is strongly dependent on the knowledge of interaction between all participating particles which is very poorly known at present. It is very important to investigate this problem because the internal structure of NS and phase transitions between regions with different composition has serious consequences, for example, for understanding scenarios of supernova models, potential sources of GW and nucleosynthesis. For example, if pions are included in the EOS used for evolution of supernovae (Mayle et al., Ap.J 418, 398 (1993)), it is suggested the electron neutrino density can increase by about 160%.
32 Threshold densities for production of hyperons Skyrme Group I Skyrme Group II Skyrme Group III A18+δv+UIX* Σ 0.29(4) no no 0.34 Λ 0.41(4) 0.80(10) no 0.47 Assumptions: non-interacting hyperons, lowest energy state in dense matter equal to vacuum rest mass, predominance of weak interactions
33 Connection with finite nuclei represents a specific nuclear physics interest: Recent trend and hope is to find new physics at the boundaries of nuclear stability with the ratio of protons and neutrons much different from unity (e.g. N/Z ~ 2-3) Neutron stars contain highly asymmetric matter N>>Z A UNIQUE EXTRAPOLATION POINT FOR POTENTIALS FITTED ALONG THE STABILITY LINE ( N ~ Z)
34 New developments EOS based on full Skyrme interaction 3D selfconsistent Hartree-Fock approximation no nuclear shape constraints (previously only spherical) natural inclusion of shell effects finite temperature Bonche and Vautherin, NP A372, 496 (1981) (1D) Magierski and Heenen, PRC 65, (2002) (T=0) In full range of relevant densities and particle compositions Comment: Codes are flexible, the Skyrme interaction can be easily replaced by any other phenomenological density dependent effective interaction (separable, Gogny etc) or some other NN potential
35 N-N potential based on quark and gluon exchange Only 2 parameters!!!! T.Barnes et al., PRC 48, 539 (1995) and TALK TOMORROW! E/A [MeV] Pure neutron matter SkO SLy230a Skyrme1' v14 +TNI Quark Quark+attract A18+δv+UIX * number density [fm -3 ] EOS for pure neutron Matter derived in the Fermi gas approximation Comments: 1. It has different density dependence 2. It is in the correct energy range 3. The attractive part of the potential is understood in principle This EOS could produce predictions up to unlimited high density
36 Conclusions 1. Unique selection of EOS may not be possible unless the nucleon-nucleon interaction in nuclear medium is fully understood 2. However constraints on the existing models should be sought and implemented 3. Systematic tests of EOS in supernova simulations may provide additional valuable constraints 4. More effects have to be investigated with successful EOS (superfluidity, magnetic fields, presence of boson condensates, mixed phases at high densities, etc) 5. New developments should be pursued
Self-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 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 informationNuclear 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 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 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 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 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 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 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 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 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 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 information4 November Master 2 APIM. Le problème à N corps nucléaire: structure nucléaire
4 November 2010. Master 2 APIM Le problème à N corps nucléaire: structure nucléaire The atomic nucleus is a self-bound quantum many-body (manynucleon) system Rich phenomenology for nuclei Mean field Which
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 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 informationCorrelations derived from modern nucleon-nucleon potentials
Correlations derived from modern nucleon-nucleon potentials H. Müther Institut für Theoretische Physik, Universität Tübingen, D-72076 Tübingen, Germany A. Polls Departament d Estructura i Costituents de
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 informationDensity dependence of the symmetry energy and the nuclear equation of state : A dynamical and statistical model perspective
Density dependence of the symmetry energy and the nuclear equation of state : A dynamical and statistical model perspective D. V. Shetty, S. J. Yennello, and G. A. Souliotis The density dependence of the
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 informationThe Nuclear Many-Body Problem
The Nuclear Many-Body Problem relativistic heavy ions vacuum electron scattering quarks gluons radioactive beams heavy few nuclei body quark-gluon soup QCD nucleon QCD few body systems many body systems
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 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 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 Landscape not fully known
Nuclear Landscape not fully known Heaviest Elements? Known Nuclei Limit of proton rich nuclei? Fission Limit? Possible Nuclei Limit of Neutron Rich Nuclei? Nuclear Radii Textbooks: R = r 00 A 1/3 1/3 I.
More information1 Introduction. 2 The hadronic many body problem
Models Lecture 18 1 Introduction In the next series of lectures we discuss various models, in particluar models that are used to describe strong interaction problems. We introduce this by discussing the
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 informationNuclear & Particle Physics of Compact Stars
Nuclear & Particle Physics of Compact Stars Madappa Prakash Ohio University, Athens, OH National Nuclear Physics Summer School July 24-28, 2006, Bloomington, Indiana 1/30 How Neutron Stars are Formed Lattimer
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 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 informationInner crust composition and transition densities
Inner crust composition and transition densities W.G.Newton 1, Bao-An Li 1, J.R.Stone 2,3 M. Gearheart 1, J. Hooker 1 1 Texas A&M University - Commerce 2 University of Oxford, UK 3 Physics Division, ORNL,
More informationarxiv:nucl-th/ v1 10 Jul 1996
Microscopic nuclear equation of state with three-body forces and neutron star structure M. Baldo, G.F. Burgio Dipartimento di Fisica, Universitá di Catania and I.N.F.N. Sezione di Catania, c.so Italia
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 informationHyperon equation of state for core-collapse simulations based on the variational many-body theory Hajime Togashi Outline
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)
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 informationCorrelating the density dependence of the symmetry y energy to neutron skins and neutron-star properties
Correlating the density dependence of the symmetry y energy to neutron skins and neutron-star properties Farrukh J Fattoyev Texas A&M University-Commerce i My TAMUC collaborators: B.-A. Li, W. G. Newton
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 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 informationMean-field concept. (Ref: Isotope Science Facility at Michigan State University, MSUCL-1345, p. 41, Nov. 2006) 1/5/16 Volker Oberacker, Vanderbilt 1
Mean-field concept (Ref: Isotope Science Facility at Michigan State University, MSUCL-1345, p. 41, Nov. 2006) 1/5/16 Volker Oberacker, Vanderbilt 1 Static Hartree-Fock (HF) theory Fundamental puzzle: The
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 informationSymmetry energy of dilute warm nuclear matter
Symmetry energy of dilute warm nuclear matter J. B. Natowitz, G. Röpke, 1 S. Typel, 2,3 D. Blaschke, 4, 5 A. Bonasera, 6 K. Hagel, T. Klähn, 4, 7 S. Kowalski, L. Qin, S. Shlomo, R. Wada, and H. H. Wolter
More informationNuclear structure Anatoli Afanasjev Mississippi State University
Nuclear structure Anatoli Afanasjev Mississippi State University 1. Nuclear theory selection of starting point 2. What can be done exactly (ab-initio calculations) and why we cannot do that systematically?
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 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 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 informationClusters in Low-Density Nuclear Matter
Clusters in Low-Density Nuclear Matter Excellence Cluster Universe, Technische Universität München GSI Helmholtzzentrum für Schwerionenforschung, Darmstadt Helmholtz International Summer School: Nuclear
More informationBao-An Li. Collaborators: Bao-Jun Cai, Lie-Wen Chen, Chang Xu, Jun Xu, Zhi-Gang Xiao and Gao-Chan Yong
Probing High-Density Symmetry Energy with Heavy-Ion Reactions Bao-An Li Collaborators: Bao-Jun Cai, Lie-Wen Chen, Chang Xu, Jun Xu, Zhi-Gang Xiao and Gao-Chan Yong Outline What is symmetry energy? Why
More informationNuclear symmetry energy deduced from dipole excitations: comparison with other constraints
Nuclear symmetry energy deduced from dipole excitations: a comparison with other constraints G. Colò June 15th, 2010 This work is part of a longer-term research plan. The goal is: understanding which are
More informationConstraining the nuclear EoS by combining nuclear data and GW observations
Constraining the nuclear EoS by combining nuclear data and GW observations Michael McNeil Forbes Washington State University (Pullman) and University of Washington A Minimal Nuclear Energy Density Functional
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 informationPhase transitions in dilute stellar matter. Francesca Gulminelli & Adriana Raduta
Phase transitions in dilute stellar matter Francesca Gulminelli & Adriana Raduta LPC Caen, France IFIN Bucharest Supernova remnant and neutron star in Puppis A (ROSAT x-ray) χ 1/2 Τ 10 12 Κ Motivation:
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 informationProbing the High-Density Behavior of Symmetry Energy with Gravitational Waves
Probing the High-Density Behavior of Symmetry Energy with Gravitational Waves Farrukh J. Fattoyev Bao-An Li, William G. Newton Texas A&M University-Commerce 27 th Texas Symposium on Relativistic Astrophysics
More informationNucelon self-energy in nuclear matter and how to probe ot with RIBs
Nucelon self-energy in nuclear matter and how to probe ot with RIBs Christian Fuchs University of Tübingen Germany Christian Fuchs - Uni Tübingen p.1/?? Outline relativistic dynamics E/A [MeV] 6 5 4 3
More informationPossibility of hadron-quark coexistence in massive neutron stars
Possibility of hadron-quark coexistence in massive neutron stars Tsuyoshi Miyatsu Department of Physics, Soongsil University, Korea July 17, 2015 Nuclear-Astrophysics: Theory and Experiments on 2015 2nd
More informationThe crust-core transition and the stellar matter equation of state
The crust-core transition and the stellar matter equation of state Helena Pais CFisUC, University of Coimbra, Portugal Nuclear Physics, Compact Stars, and Compact Star Mergers YITP, Kyoto, Japan, October
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 informationModeling the EOS. Christian Fuchs 1 & Hermann Wolter 2. 1 University of Tübingen/Germany. 2 University of München/Germany
Modeling the EOS Christian Fuchs 1 & Hermann Wolter 2 1 University of Tübingen/Germany 2 University of München/Germany Christian Fuchs - Uni Tübingen p.1/20 Outline Christian Fuchs - Uni Tübingen p.2/20
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 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 informationQuantum Theory of Many-Particle Systems, Phys. 540
Quantum Theory of Many-Particle Systems, Phys. 540 Questions about organization Second quantization Questions about last class? Comments? Similar strategy N-particles Consider Two-body operators in Fock
More informationThe isospin dependence of the nuclear force and its impact on the many-body system
Journal of Physics: Conference Series OPEN ACCESS The isospin dependence of the nuclear force and its impact on the many-body system To cite this article: F Sammarruca et al 2015 J. Phys.: Conf. Ser. 580
More informationBetty Tsang, NSCL/MSU 曾敏兒. collaboration
Science of the SpRIT Time Projection Chamber From Earth to Heavens: Femto-scale nuclei to Astrophysical objects SAMURAI International Collaboration Meeting, Sept 8-9, 2014 Sendai, Japan 曾敏兒 for Betty Tsang,
More informationSome new developments in relativistic point-coupling models
Some new developments in relativistic point-coupling models T. J. Buervenich 1, D. G. Madland 1, J. A. Maruhn 2, and P.-G. Reinhard 3 1 Los Alamos National Laboratory 2 University of Frankfurt 3 University
More informationc E If photon Mass particle 8-1
Nuclear Force, Structure and Models Readings: Nuclear and Radiochemistry: Chapter 10 (Nuclear Models) Modern Nuclear Chemistry: Chapter 5 (Nuclear Forces) and Chapter 6 (Nuclear Structure) Characterization
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 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 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 informationParity-Violating Asymmetry for 208 Pb
Parity-Violating Asymmetry for 208 Pb Matteo Vorabbi Dipartimento di Fisica - Università di Pavia INFN - Sezione di Pavia Rome - 2015 January 15 Matteo Vorabbi (Università di Pavia) Parity-Violating Asymmetry
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 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 informationNucleon Nucleon Forces and Mesons
Canada s ational Laboratory for Particle and uclear Physics Laboratoire national canadien pour la recherche en physique nucléaire et en physique des particules ucleon ucleon Forces and Mesons Sonia Bacca
More informationGround State Properties of Closed Shell 4 He Nucleus under Compression
Journal of Applied Mathematics and Physics, 2018, 6, 458-467 http://www.scirp.org/journal/jamp ISSN Online: 2327-4379 ISSN Print: 2327-4352 Ground State Properties of Closed Shell 4 He Nucleus under Compression
More informationProperties of Nuclei deduced from the Nuclear Mass
Properties of Nuclei deduced from the Nuclear Mass -the 2nd lecture- @Milano March 16-20, 2015 Yoshitaka Fujita Osaka University Image of Nuclei Our simple image for Nuclei!? Nuclear Physics by Bohr and
More informationStructure and propermes of nuclear ma3er in compact stars
Structure and propermes of nuclear ma3er in compact stars Toshiki Maruyama (JAEA) Nobutoshi Yasutake (Chiba Inst. of Tech.) Minoru Okamoto (Univ. of Tsukuba & JAEA) Toshitaka Tatsumi (Kyoto Univ.) Low-
More informationCore-collapse supernova simulations in three dimensions
Core-collapse supernova simulations in three dimensions Eric J Lentz University of Tennessee, Knoxville S. Bruenn (FAU), W. R. Hix (ORNL/UTK), O. E. B. Messer (ORNL), A. Mezzacappa (UTK), J. Blondin (NCSU),
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 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 informationRelativistic Mean Field Model for finite nuclei and infinite matter
Relativistic Mean Field Model for finite nuclei and infinite matter Hiroshi Toki (RCNP/Osaka) in collaboration with H. Shen (Nankai/China) L. Geng (Beijing/China) K. Sumiyoshi (Numazu) Supernova explosion
More informationGravitational waves (...and GRB central engines...) from neutron star mergers
Gravitational waves (...and GRB central engines...) from neutron star mergers Roland Oechslin MPA Garching, SFB/TR 7 Ringberg Workshop, 27.3.2007 In this talk: -Intro: -Overview & Motivation -Neutron star
More informationUltracold atoms and neutron-rich matter in nuclei and astrophysics
Ultracold atoms and neutron-rich matter in nuclei and astrophysics Achim Schwenk NORDITA program Pushing the boundaries with cold atoms Stockholm, Jan. 23, 2013 Outline Advances in nuclear forces 3N forces
More informationIntroduction to Nuclear Physics
1/3 S.PÉRU The nucleus a complex system? What is the heaviest nucleus? How many nuclei do exist? What about the shapes of the nuclei? I) Some features about the nucleus discovery radius, shape binding
More informationNeutron skin measurements and its constraints for neutron matter. C. J. Horowitz, Indiana University INT, Seattle, 2016
Neutron skin measurements and its constraints for neutron matter C. J. Horowitz, Indiana University INT, Seattle, 2016 1 Neutron Rich Matter Compress almost anything to 10 11 + g/cm 3 and electrons react
More informationQuantum mechanics of many-fermion systems
Quantum mechanics of many-fermion systems Kouichi Hagino Tohoku University, Sendai, Japan 1. Identical particles: Fermions and Bosons 2. Simple examples: systems with two identical particles 3. Pauli principle
More informationCrust-core transitions in neutron stars revisited
Crust-core transitions in neutron stars revisited X. Viñas a, C. González-Boquera a, B.K. Sharma a,b M. Centelles a a Departament de Física Quàntica i Astrofísica and Institut de Ciències del Cosmos, Universitat
More informationA survey of the relativistic mean field approach
A survey of the relativistic mean field approach B. D. Serot and J. D. Walecka, The relativistic nuclear many body problem. Adv. Nuc. Phys., 16:1, 1986. Non relativistic mean field Small potentials (a
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 informationarxiv:astro-ph/ v2 24 Apr 2001
Neutron Star Structure and the Neutron Radius of 208 Pb C. J. Horowitz Nuclear Theory Center and Dept. of Physics, Indiana University, Bloomington, IN 47405 J. Piekarewicz Department of Physics Florida
More informationNeutron Rich Nuclei in Heaven and Earth
First Prev Next Last Go Back Neutron Rich Nuclei in Heaven and Earth Jorge Piekarewicz with Bonnie Todd-Rutel Tallahassee, Florida, USA Page 1 of 15 Cassiopeia A: Chandra 08/23/04 Workshop on Nuclear Incompressibility
More informationFinite Range Force models for EOS
1 / 30 Finite Range Force models for EOS INT 2012-2a Core-collapse supernova Yeunhwan Lim 1 (in collaboration with Prof. James M. Lattimer 1 ) 1 SUNY STONY BROOK, NY 11794 July 11, 2012 2 / 30 Table of
More informationPhysics 228 Today: April 22, 2012 Ch. 43 Nuclear Physics. Website: Sakai 01:750:228 or
Physics 228 Today: April 22, 2012 Ch. 43 Nuclear Physics Website: Sakai 01:750:228 or www.physics.rutgers.edu/ugrad/228 Nuclear Sizes Nuclei occupy the center of the atom. We can view them as being more
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 informationPREX and CREX. R N from Electroweak Asymmetry in Elastic Electron-Nucleus Scattering. Neutron Skin.
http://hallaweb.jlab.org/parity/prex PREX and CREX 08 Pb Horowitz 48 Ca Neutron Skin R N from Electroweak Asymmetry in Elastic Electron-Nucleus Scattering R L 4 6 A ~ 10 PV Q ~ 10 R L PRL 108 (01) 1150
More informationarxiv:astro-ph/ v1 16 Apr 1999
PHASE TRANSITIONS IN NEUTRON STARS AND MAXIMUM MASSES H. HEISELBERG Nordita, Blegdamsvej 17, DK-2100 Copenhagen Ø, Denmark and arxiv:astro-ph/9904214v1 16 Apr 1999 M. HJORTH-JENSEN Department of Physics,
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 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 informationStructure of Atomic Nuclei. Anthony W. Thomas
Structure of Atomic Nuclei Anthony W. Thomas JLab Users Meeting Jefferson Lab : June 2 nd 2015 The Issues What lies at the heart of nuclear structure? Start from a QCD-inspired model of hadron structure
More informationQuantum Theory of Many-Particle Systems, Phys. 540
Quantum Theory of Many-Particle Systems, Phys. 540 IPM? Atoms? Nuclei: more now Other questions about last class? Assignment for next week Wednesday ---> Comments? Nuclear shell structure Ground-state
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 informationNeutron Skins with α-clusters
Neutron Skins with α-clusters GSI Helmholtzzentrum für Schwerionenforschung, Darmstadt Nuclear Astrophysics Virtual Institute Hirschegg 2015 Nuclear Structure and Reactions: Weak, Strange and Exotic International
More informationThe Nuclear Equation of State
The Nuclear Equation of State Theoretical models for nuclear structure studies Xavier Roca-Maza Università degli Studi di Milano e INFN, sezione di Milano Terzo Incontro Nazionale di Fisica Nucleare LNF,
More information