Quantum simula+ons of nuclear pasta
|
|
|
- Meagan Paul
- 5 years ago
- Views:
Transcription
1 Quantum simula+ons of nuclear pasta William Newton, Sarah Cantu, Mike Gearheart, Farrukh Fa=oyev, Bao-An Li Texas A&M University-Commerce Jirina Rikovska Stone, Helena Pais, Alex Kaltenborn University of Tennessee INT, Aug 1, 2016
2 Frustra+on leads to pasta forma+on at the base of the inner crust Outer Crust Pasta: Ravenhall, Pethick and Wilson Phys. Rev. Le=. 50, 2066, 1983 a^er all, the cooking of spaghe_, while it spoils the perfect straightness of the strands, does not destroy the characteris+c short range order Wa=s et al, arxiv: &"neutron"+"proton"fluid" Pasta" Inverted"pasta"(bubbles)" "&"Pure"neutron"(super)fluid" 100&1200"m"" 25" "250"m" 5" "30"m" Surface Outer"Crust" Core" 11" g"cm &3 " 14" g"cm &3 " &1.8"x"10 14" g"cm &3 " Inner"Crust" Mantle"
3 Pasta phenomenologically similar to terrestrial so^ condensed ma=er
4 Pasta phenomenologically similar to terrestrial so^ condensed ma=er
5 Pasta phenomenologically similar to terrestrial so^ condensed ma=er
6 Pasta phenomenologically similar to terrestrial so^ condensed ma=er A wide range of mechanical properties are exhibited (liquid crystal Pethick, Potehkin, Phys Lett B427, 1998) See Caplan,Horowitz arxiv:
7 Modeling pasta Semi-classical: Compressible Liquid Drop model (BBP 1971) Thomas-Fermi (Buchler&Barkat, PRL27, 1971) Molecular Dynamics (Maruyama+, PRC57, 1998) (400,000+ nucleons, e.g. Schneider+, PRC93, 2016) Quantum: Hartree-Fock (Negele&Vautherin, NPhysA207, 1973) nucleons Surface term Coulomb term Nucleus x, n r N Volume (Bulk) term Neutron & electron Gas n n
8 Systema+c EOS modeling Use our best calcula+ons of PNM proper+es to constrain our EOS models. 2 purely isovector parameters in Skyrme and RMF energy density func+onals allows us to take a baseline model and refit those two parameters to PNM data Polytropes above 1.5n 0 tuned to give desired max mass 2+M sun Gandolfi, Gezerlis, Carlson, ARNPS 65 (2015) Fa=oyev, Newton, Xu, Li, PRC86, (2012) Brown, Schwenk, PRC89, (2014)
9 How much pasta is there? Newton, Fa=oyev, in prep. 100&1200"m"" 25" "250"m" 5" "30"m" "&"Pure"neutron"(super)fluid" &"neutron"+"proton"fluid" Pasta" Inverted"pasta"(bubbles)" Outer"Crust" Core" 11" g"cm &3 " 14" g"cm &3 " &1.8"x"10 14" g"cm &3 " Inner"Crust" Mantle"
10 3D Hartree-Fock Simula+ons of Pasta Shell structure of unbound neutrons (sca=ering from Pasta structures) means many low-lying energy minima (Quantum frustra+on) Disordered, amorphous (Magierski & Heenen PRC ) Fermionic Casimir Effect, effec+ve a=rac+on between certain structures
11 3D Hartree-Fock Simula+ons of Pasta Finite Temperature, y p = 0.3; Newton+, PhD Thesis, Jphys Conf Series 46, 2006; PRC , 2009 Amphiphilic Bicon+nuous Cubic-P Phase
12 3D Hartree-Fock Simula+ons of Pasta SLy4 Gögelein&Müther, PRC , 2007 Skyrme and RMF simula+ons
13 3D Hartree-Fock Simula+ons of Pasta y p = Guiding poten+als to obtain gyroid shapes Schuetrumpf+ PRC , 2015; , PRC 2015
14 3D Hartree-Fock: Boundary Condi+ons Newton+, PhD Thesis, Jphys Conf Series 46, 2006; PRC , 2009
15 3D Hartree-Fock: Boundary Condi+ons Newton+, PhD Thesis, Jphys Conf Series 46, 2006; PRC , 2009
16 3D Hartree-Fock: Boundary Condi+ons spurious shell effects Solu+on: average over Bloch momentum covectors Schuetrumpf , PRC 2015
17 Pasta in hot, proton rich ma=er y p = 0.3 T = 10 MeV T = 2 MeV Newton, Stone, PRC , 2009; Pais, Newton, PRL , 2012 Pais, Newton, Stone PRC , 2014
18 Pasta in hot, proton rich ma=er y p = 0.3 T = 2 MeV Pais+, PRL , 2012
19 Pasta in hot, proton rich ma=er y p = 0.3 T=6MeV T=2MeV Pais, Newton, Stone, PRC , 2014
20 Pasta in hot, proton rich ma=er y p = 0.3 Pais, Newton, Stone, PRC , 2014
21 Pasta in hot, proton rich ma=er y p = 0.3 Pais, Newton, Stone, PRC , 2014
22 Pasta transi+ons in the neutron star crust NRAPR, y p = ; Pasta starts appearing at n b 0.04 fm fm fm fm fm fm fm fm fm fm fm -3 Newton, Stone, Kaltenborn, in prep
23 Disordered pasta Prolate: γ=0 o Increasingly deformed with β Spherical: β=0 Oblate: γ=60 o Increasingly deformed with β Newton, Kaltenborn and Stone, in prep
24 Disordered pasta Prolate: γ=0 o Increasingly deformed with β Spherical: β=0 Prolate: γ=0 o Increasingly deformed with β Minima separated by energy barriers <10 kev/par+cle As mantle cools below K, pasta phases may organize into microscopic domains containing different geometries coexis+ng at the same density Highly disordered Newton, Kaltenborn and Stone, in prep
25 SkIUFSU; L = 30 MeV; nsph-pasta = fm-3; ncc = fm fm fm fm fm fm fm fm fm fm-3
26 NRAPR L = 60 MeV; nsph-pasta = fm-3; ncc = fm fm fm fm fm fm fm fm fm-3
27 SkIUFSU; L = 90 MeV; nsph-pasta = fm-3; ncc = fm fm fm fm fm fm fm fm-3
28 Transi+on pressures Core Pasta phases CLDM Fa=oyev, Newton, Xu, Li, PRC86, (2012) Newton & Fa=oyev, in prep. Newton, Stone, Kaltenborn, in prep.
29 Transi+on pressures Core Pasta phases CLDM 3DHF Fa=oyev, Newton, Xu, Li, PRC86, (2012) Newton & Fa=oyev, in prep. Newton, Stone, Kaltenborn, in prep.
30 Pasta mass frac+on CLDM 3DHF predicts over 50%
31 Pasta mass frac+on CLDM 3DHF 3DHF predicts over 50%
32 Calibra+ng CLDM using 3DHF y p = 0.02 n b = fm -3 n b = fm -3 NRAPR (L=60 MeV)
33 Calibra+ng CLDM using 3DHF y p = 0.02 n b = fm -3 n b = fm -3 SkIUFSU (L=30 MeV)
34 How well do we know the crust? Newton, Gearheart, Li, ApJS 204, 2013
35 How well do we know the crust? Newton, Gearheart, Li, ApJS 204, 2013
36 Long range order of pasta
37 Long range order at pasta freezing point L NRAPR a (See Watanabe+, NPhysA 676, 2003)
38 Conclusions and open ques+ons Quantum predicts larger region of pasta ma=er than semi-classical methods (shell effects) Pasta mass of crust > 50% Effect of symmetry energy indirect through equilibrium proton frac+on Magne+c field ordering? Anisotropic transport proper+es Importance of various types of disorder (what happens as pasta cools? - topological defects - quantum frustra+on - thermodynamic fluctua+ons
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
Inner 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,
Neutron star Equa-ons of State: An ideal to aim towards
Neutron star Equa-ons of State: An ideal to aim towards Astrophysical modeling generally requires EOS tables more extensive than tradi-onal pressure versus energy density: Chemical poten-als, density-
E. 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
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
Dense 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
Dense 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
Constraining 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
Introduction to Dense Matter. C. J. Pethick (U. of Copenhagen and NORDITA)
Introduction to Dense Matter C. J. Pethick (U. of Copenhagen and NORDITA) Astro-Solids, Dense Matter, and Gravitational Waves INT, Seattle, April 16, 2018 Bottom lines Exciting time for neutron star studies:
Nuclear 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
Fermi sea. λ F. (non-interacting particles)
Fermi sea λ F F (non-interacting particles) a Fermi sea λf Fermi sea λf a Fermi sea λf a a Fermi sea λf Question: What is the most favorable arrangement of these two spheres? a R=? a Answer: The energy
Crust-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
Nuclear 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,
Nuclear 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
Observables predicted by HF theory
Observables predicted by HF theory Total binding energy of the nucleus in its ground state separation energies for p / n (= BE differences) Ground state density distribution of protons and neutrons mean
Structure 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-
Neutron matter from chiral effective field theory interactions
Neutron matter from chiral effective field theory interactions Ingo Tews, In collaboration with K. Hebeler, T. Krüger, A. Schwenk, JINA Neutron Stars, May 26, 2016, Athens, OH Chiral effective field theory
Neutron-star properties with unified equations of state
Neutron-star properties with unified equations of state Nicolas Chamel in collaboration with J. M. Pearson, S. Goriely, A. F. Fantina Institute of Astronomy and Astrophysics Université Libre de Bruxelles,
Nuclear 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
Few-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
Clusters 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
Microscopic Fusion Dynamics Based on TDHF
Dynamical Approach Microscopic Fusion Dynamics Based on TDHF FISSION FUSION Calculate PES as a function of nuclear shape Microscopic HF, HFB, RMF + constraints e.g. Q20, Q30, Q40 as H + lql0 Macroscopic-Microscopic
arxiv: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
The 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
Probing 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
Alex Gezerlis. New Ideas in Constraining Nuclear Forces ECT*, Trento, Italy June 5, 2018
Quantum Monte Carlo interactions with From microscopic to effective Chiral Effective Field Theory Interactions using Quantum Monte Carlo Alex Gezerlis New Ideas in Constraining Nuclear Forces ECT*, Trento,
Correlating 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
Neutron-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
Equation 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,
Bao-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
arxiv: v1 [astro-ph.sr] 9 Dec 2011
![arxiv: v1 [astro-ph.sr] 9 Dec 2011](/thumbs/86/94765335.jpg "arxiv: v1 [astro-ph.sr] 9 Dec 2011")
Symmetry energy, inner crust and global modeling 1 Chapter 1 arxiv:1112.2018v1 [astro-ph.sr] 9 Dec 2011 THE NUCLEAR SYMMETRY ENERGY, THE INNER CRUST, AND GLOBAL NEUTRON STAR MODELING W.G. Newton, M. Gearheart,
Functional 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
Lisheng Geng. Ground state properties of finite nuclei in the relativistic mean field model
Ground state properties of finite nuclei in the relativistic mean field model Lisheng Geng Research Center for Nuclear Physics, Osaka University School of Physics, Beijing University Long-time collaborators
Neutron 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
Structure properties of medium and heavy exotic nuclei
Journal of Physics: Conference Series Structure properties of medium and heavy exotic nuclei To cite this article: M K Gaidarov 212 J. Phys.: Conf. Ser. 381 12112 View the article online for updates and
Nuclear 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
An 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
Three-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
Neutron 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:
User s Guide for Neutron Star Matter EOS
User s Guide for Neutron Star Matter EOS CQMC model within RHF approximation and Thomas-Fermi model Tsuyoshi Miyatsu (Tokyo Univ. of Sci.) Ken ichiro Nakazato (Kyushu University) May 1 2016 Abstract This
Constraints on neutron stars from nuclear forces
Constraints on neutron stars from nuclear forces Achim Schwenk Workshop on the formation and evolution of neutron stars Bonn, Feb. 27, 2012 Main points Advances in nuclear forces and nuclear matter theory
Thermodynamic properties of nuclear pasta in neutron star crusts
Thermodynamic properties of nuclear pasta in neutron star crusts Gentaro Watanabe a, Kei Iida a,b, Katsuhiko Sato a,c a Department of Physics, University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo 113-0033,
The 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
Some 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
Relativistic versus Non Relativistic Mean Field Models in Comparison
Relativistic versus Non Relativistic Mean Field Models in Comparison 1) Sampling Importance Formal structure of nuclear energy density functionals local density approximation and gradient terms, overall
Current 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,
Simula'ons of the Neutron Star Crust
CSQCD V, l Aquila 2016 Simula'ons of the Neutron Star Crust general remarks on NS and crust modeling approach nuclear ma5er and nuclei inner crust pasta phase what s next R. Nandi, SWS FIAS Frankfurt structure
The 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
Nuclear 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
Pure Neutron Matter Constraints and Nuclear Symmetry Energy
Journal of Physics: Conference Series Pure Neutron Matter Constraints and Nuclear Symmetry Energy To cite this article: F J Fattoyev et al 2013 J. Phys.: Conf. Ser. 420 012108 View the article online for
neutron star basics λ. λ
neutron star basics A solar mass consists of ~ 10 57 nucleons. If they are separated by typical inter-nucleon distances, what would the radius of the volume containing them be? neutron star basics ( )
文德华 Department of Physics, South China Univ. of Tech. ( 华南理工大学物理系 )
Investigation on the oscillation modes of neutron stars 文德华 Department of Physics, South China Univ. of Tech. ( 华南理工大学物理系 ) collaborators Bao-An Li, William Newton, Plamen Krastev Department of Physics
arxiv: v1 [nucl-th] 30 Mar 2015
![arxiv: v1 [nucl-th] 30 Mar 2015](/thumbs/83/88958643.jpg "arxiv: v1 [nucl-th] 30 Mar 2015")
Compact Stars in the QCD Phase Diagram IV (CSQCD IV) September 26-30, 2014, Prerow, Germany http://www.ift.uni.wroc.pl/~csqcdiv Core-collapse supernova matter: light clusters, pasta phase and phase transitions
Hartree-Fock-Bogoliubov atomic mass models and the description of the neutron-star crust
Hartree-Fock-Bogoliubov atomic mass models and the description of the neutron-star crust Nicolas Chamel in collaboration with S. Goriely and J. M. Pearson Research Associate FNRS Institute of Astronomy
Constraining 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.
Symmetry 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
b - 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
THE NEUTRON STAR CRUST AND SURFACE WORKSHOP. Quantum calculation of nucleus-vortex interaction in the inner crust of neutron stars
THE NEUTRON STAR CRUST AND SURFACE WORKSHOP Seattle 25-29 June 2007 Quantum calculation of nucleus-vortex interaction in the inner crust of neutron stars P. Avogadro, F.Barranco, R.A.Broglia, E.Vigezzi
Ultracold 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
Density distributions of superheavy nuclei
PHYSICAL REVIEW C 71, 3432 (5) Density distributions of superheavy nuclei J. C. Pei, 1 F. R. Xu, 1,2,3, and P. D. Stevenson 4 1 School of Physics, Peking University, Beijing 1871, China 2 Institute of
Quantum Monte Carlo with
Quantum Monte Carlo with QuantumField Monte Carlo Interactions with Chiral Effective Theory Chiral Effective Field Theory Interactions From matter to nuclei Alexandros Gezerlis ECT*-EMMI Workshop Neutron-Rich
Evolution Of Shell Structure, Shapes & Collective Modes. Dario Vretenar
Evolution Of Shell Structure, Shapes & Collective Modes Dario Vretenar vretenar@phy.hr 1. Evolution of shell structure with N and Z A. Modification of the effective single-nucleon potential Relativistic
Theory of neutron-rich nuclei and nuclear radii Witold Nazarewicz (with Paul-Gerhard Reinhard) PREX Workshop, JLab, August 17-19, 2008
Theory of neutron-rich nuclei and nuclear radii Witold Nazarewicz (with Paul-Gerhard Reinhard) PREX Workshop, JLab, August 17-19, 2008 Introduction to neutron-rich nuclei Radii, skins, and halos From finite
From neutrons to atoms (in 2D) and back
From neutrons to atoms (in 2D) and back Alex Gezerlis Exploring nuclear physics with ultracold atoms workshop ECT*, Trento, Italy June 18, 2018 Outline Motivation Credit: Dany Page 2D cold gases Static
Ground-state properties of some N=Z medium mass heavy nuclei. Keywords: Nuclear properties, neutron skin thickness, HFB method, RMF model, N=Z nuclei
Ground-state properties of some N=Z medium mass heavy nuclei Serkan Akkoyun 1, Tuncay Bayram 2, Şevki Şentürk 3 1 Department of Physics, Faculty of Science, Cumhuriyet University, Sivas, Turkey 2 Department
On single nucleon wave func0ons. Igal Talmi The Weizman Ins0tute of Science Rehovot, Israel
On single nucleon wave func0ons Igal Talmi The Weizman Ins0tute of Science Rehovot, Israel The main success of the nuclear shell model Nuclei with magic numbers of protons and neutrons exhibit extra stability.
Superfluid Heat Conduction in the Neutron Star Crust
Superfluid Heat Conduction in the Neutron Star Crust Sanjay Reddy Los Alamos National Lab Collaborators : Deborah Aguilera Vincenzo Cirigliano Jose Pons Rishi Sharma arxiv:0807.4754 Thermal Conduction
GENERALIZED 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
Low energy effec,ve theories for metals. Sung-Sik Lee McMaster University Perimeter Ins,tute
Low energy effec,ve theories for metals Sung-Sik Lee McMaster University Perimeter Ins,tute Goal of many-body physics : to extract a small set of useful informa,on out of a large number of degrees of freedom
Impact of Terrestrial Facilities on the Structure of the Neutron Star Crust
Impact of Terrestrial Facilities on the Structure of the Neutron Star Crust Jorge Piekarewicz Florida State University The Neutron Star Crust and Surface (INT - June, 2007) My Collaborators: C.J. Horowitz,
Collective excitations of Λ hypernuclei
Collective excitations of Λ hypernuclei Kouichi Hagino (Tohoku Univ.) J.M. Yao (Southwest Univ.) Z.P. Li (Southwest Univ.) F. Minato (JAEA) 1. Introduction 2. Deformation of Lambda hypernuclei 3. Collective
PoS(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,
Fermionic molecular dynamics
Fermionic molecular dynamics Can it cook nuclear pasta? K. Vantournhout H. Feldmeier GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany NuSTAR seminar April 25, 2012 Klaas Vantournhout
Astromaterial Science and Nuclear Pasta
Astromaterial Science and Nuclear Pasta M. E. Caplan and C. J. Horowitz Center for Exploration of Energy and Matter and Department of Physics, Indiana University, Bloomington, IN 47405, USA (Dated: June
4 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
The 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,
Renormalization group methods in nuclear few- and many-body problems
Renormalization group methods in nuclear few- and many-body problems Lecture 3 S.K. Bogner (NSCL/MSU) 2011 National Nuclear Physics Summer School University of North Carolina at Chapel Hill Lecture 2 outline
Quantum 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,
arxiv: v1 [nucl-th] 21 Aug 2007
![arxiv: v1 [nucl-th] 21 Aug 2007](/thumbs/84/89190376.jpg "arxiv: v1 [nucl-th] 21 Aug 2007")
Symmetry Energy as a Function of Density and Mass Pawel Danielewicz and Jenny Lee arxiv:0708.2830v1 [nucl-th] 21 ug 2007 National Superconducting Cyclotron Laboratory and Department of Physics and stronomy,
Collective excitations of Lambda hypernuclei
Collective excitations of Lambda hypernuclei Kouichi Hagino (Tohoku Univ.) Myaing Thi Win (Lashio Univ.) J.M. Yao (Southwest Univ.) Z.P. Li (Southwest Univ.) 1. Introduction 2. Deformation of Lambda hypernuclei
Nuclear density functional theory from low energy constants: application to cold atoms and neutron matter. Denis Lacroix. Outline:
Celebration of X. Viñas retirement, Milano 19-20 Sept. 2017 Nuclear density functional theory from low energy constants: application to cold atoms and neutron matter Outline: Denis Lacroix Brief historical
RFSS: Lecture 8 Nuclear Force, Structure and Models Part 1 Readings: Nuclear Force Nuclear and Radiochemistry:
RFSS: Lecture 8 Nuclear Force, Structure and Models Part 1 Readings: Nuclear and Radiochemistry: Chapter 10 (Nuclear Models) Modern Nuclear Chemistry: Chapter 5 (Nuclear Forces) and Chapter 6 (Nuclear
Shape of Lambda Hypernuclei within the Relativistic Mean-Field Approach
Universities Research Journal 2011, Vol. 4, No. 4 Shape of Lambda Hypernuclei within the Relativistic Mean-Field Approach Myaing Thi Win 1 and Kouichi Hagino 2 Abstract Self-consistent mean-field theory
c 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
What did you learn in the last lecture?
What did you learn in the last lecture? Charge density distribution of a nucleus from electron scattering SLAC: 21 GeV e s ; λ ~ 0.1 fm (to first order assume that this is also the matter distribution
Fusion and other applications of density-constrained TDDFT
Fusion and other applications of density-constrained TDDFT Volker E. Oberacker and A. Sait Umar Vanderbilt University Nashville, Tennessee, USA Collaborators: J.A. Maruhn, P.-G. Reinhard, C. Horowitz,
Symmetry energy and composition of the outer crust of neutron stars
IL NUOVO CIMENTO 39 C (2016) 400 DOI 10.1393/ncc/i2016-16400-1 Colloquia: IWM-EC 2016 Symmetry energy and composition of the outer crust of neutron stars A. F. Fantina( 1 )( 2 ),N.Chamel( 2 ),J.M.Pearson(
1 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
Strong interaction in the nuclear medium: new trends Effective interactions and energy functionals: applications to nuclear systems I
École Joliot-Curie 27 September - 3 October 2009 Lacanau - France Strong interaction in the nuclear medium: new trends Effective interactions and energy functionals: applications to nuclear systems I Marcella
Alexandros Gezerlis. Proton-neutron pairing and alpha-like quartet correlations in nuclei Workshop ECT*, Trento September 19, 2016
Quantum Monte Carlo with Pairing from cold atoms Chiral Effectivestars Fieldand Theory Interactions to neutron heavy nuclei Alexandros Gezerlis Proton-neutron pairing and alpha-like quartet correlations
Minimal Surfaces in Nuclear Pasta with the Time-Dependent Hartree-Fock Approach
Minimal Surfaces in Nuclear Pasta with the Time-Dependent Hartree-Fock Approach Bastian Schuetrumpf Institut für Theoretische Physik, Universität Frankfurt, D-60438 Frankfurt, Germany E-mail: schuetrumpf@th.physik.uni-frankfurt.de
Mean field studies of odd mass nuclei and quasiparticle excitations. Luis M. Robledo Universidad Autónoma de Madrid Spain
Mean field studies of odd mass nuclei and quasiparticle excitations Luis M. Robledo Universidad Autónoma de Madrid Spain Odd nuclei and multiquasiparticle excitations(motivation) Nuclei with odd number
The 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
Shape coexistence and beta decay in proton-rich A~70 nuclei within beyond-mean-field approach
Shape coexistence and beta decay in proton-rich A~ nuclei within beyond-mean-field approach A. PETROVICI Horia Hulubei National Institute for Physics and Nuclear Engineering, Bucharest, Romania Outline
Nuclear Energy Density Functional
UNEDF Project: Towards a Universal Nuclear Energy Density Functional Atomic nucleus Piotr Magierski Warsaw University of Technology/University of Washington Nuclear Landscape 126 superheavy nuclei protons
Equation 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
arxiv: v2 [nucl-th] 13 Apr 2012
![arxiv: v2 [nucl-th] 13 Apr 2012](/thumbs/83/88567993.jpg "arxiv: v2 [nucl-th] 13 Apr 2012")
Nuclear pasta in supernovae and neutron stars 1 Chapter 1 arxiv:1109.3511v2 [nucl-th] 13 Apr 2012 NUCLEAR PASTA IN SUPERNOVAE AND NEUTRON STARS Gentaro Watanabe 1,2,3 and Toshiki Maruyama 4 1 Asia Pacific
Momentum dependence of symmetry energy
Momentum dependence of symmetry energy Joint DNP of APS & JPS October 7-11, 2014 Kona, HI, USA 曾敏兒 Betty Tsang, NSCL/MSU Equation of State of Asymmetric Nuclear Matter E/A (, ) = E/A (,0) + 2 S( ) = (
Effect of Λ(1405) on structure of multi-antikaonic nuclei
12th International Conference on Meson-Nucleon Physics and the Structure of the Nucleon, (May 31-June 4, 2010, College of William and Mary, Williamsburg, Virginia) Session 2B Effect of Λ(1405) on structure
Symmetry Energy. in Structure and in Central and Direct Reactions
: in Structure and in Central and Direct Reactions Pawel Natl Superconducting Cyclotron Lab, US The 12 th International Conference on Nucleus-Nucleus Collisions June 21-26, 2015, Catania, Italy Bulk Properties