QCD Structure of Hadronic Matter

Transcription

1 QCD Structure of Hadronic Matter Hadron Nucleus Neutron star r ~1 [fm] r ~10 [fm] r ~10 [km] Light Quarks m u ~ 2 MeV m d ~ 5 MeV m s ~ 90 MeV I II III Heavy Quarks m c ~ 1.3 GeV m b ~ 4.2 GeV m t ~ 171 GeV T. Hatsuda (U. Tokyo/RIKEN) Feb.6 (2012) at Yukawa Symposium

2 Modern challenges in Hadron Physics Primordial form of matter quark-gluon plasma Origin of heavy elements in explosive astrophysical phenomena Super dense matter neutron star, exotic matter, New physics search dark matter,

3 Contents [1] Introduction [2] Precision Lattice QCD [3] Hot QCD [4] Dense QCD [5] Nuclear Force from QCD [6] Dense QCD and Ultra-cold Atoms [7] Summary

4 Quantum Chromo Dynamics Nambu (1966) Running masses: m q (Q) Running coupling: α s (Q)=g 2 /4π quark masses (from lattice QCD) [MeV] 2GeV) m u 2.19(15) m d 4.67(20) m s 94(3) FLAG working group, arxiv: [hep-lat] Bethke, Eur. Phys. J C(2009)64:689

5 ~0.2 GeV Schematic QCD phase diagram Quark-Gluon Plasma Chiral Superfluid Nuclear Superfluid Color Superconductivity ~1 GeV

6 Symmetry realization in massless QCD(N c =3, N f =3) Cabibbo and Parisi, PLB 59 (1975); Collins & Perry, PRL 34 (1975) QGP : SU C ( 3) [ SU L(3) SU R(3)] UB(1) QGP Fermi csf : qq 0 SU (3) SU (3) U (1) C L R B CSC : SU C L R qq 0 (3) Z(2) Dirac Nambu, PRL 4 (1960) Dirac mass Alford, Rajagopal & Wilczek, NP B537 (1999) Majorana mass

7 ~0.2 GeV Schematic QCD phase diagram Quark-Gluon Plasma Chiral Superfluid Asakawa-Yazaki NPA (1989) Nuclear Superfluid ~1 GeV Color Superconductivity

8 QCD phase 2011 K. Fukushima and T. Hatsuda, The Phase Diagram of Dense QCD Rep. Prog. Phys. 74 (2011) High T critical point: Asakawa & Yazaki, NPA (1989) Low T critical point: Kitazawa, Koide, Kunihiro & Nemoto, PTP (2002) Hatsuda, Tachibana, Yamamto & Baym, PRL (2006)

9 space Lattice QCD Color SU(3) gauge theory for strong interaction (Nambu 1966) Asymptotic freedom (Gross & Wilczek, Politzer 1973) Lattice gauge theory (Wilson 1974) Typically sites x x L a quarks q(n) Euclidean time gluons U μ (n) O well defined statistical system (finite a and L) gauge invariant fully non-perturbative Monte Carlo simulations (Creutz 1980)

10 V(R) - 2m HL [lattice unit] Quark Confinement Q Heavy Q-Qbar potential Q after before 0.5fm 1fm 1.5fm R [lattice unit] SESAM Coll., Phys.Rev.D71 ( 05) Bali et al., Nucl.Phys.Proc.Suppl. 153 ( 06)

11 Precision Lattice QCD

12 Three limits L -1 L -1 0 (thermodynamics limit) : finite size scaling a 0 (continuum limit) : asymptotic freedom m 0 (chiral limit) : chiral pert. theory X a Techniques m ud Fermions: Staggered, Wilson, Domain-wall, Overlap different ways of handling chiral symmetry Improved actions: stout, HEX, asktad, HISQ, clover,. different ways of reducing the discretization error Advanced algorithms: RHMC, DDHMC, LMA,. techniques to make the simulations fast and reliable 3-flavor (2+1)-flavor (1+1+1)-flavor

13 QCD running coupling world average (exp. only) α s (M z )=0.1186(11) world average (lattice only) α s (M z )=0.1189(5) Summary by Shintani (Lattice2011)

14 N f =2+1 N f =2 N f =0 ssbar content of the proton Takeda [JLQCD Coll.], PRD 83 (2011) Giedt, Thomas, Young PRL103(2009)

15 σ SI [pb] WIMP Nucleon Interaction Giedt, Thomas, Young Phys. Rev. Lett. 103 (2009) Σ πn [MeV] XENON100 Coll.: Phys.Rev.Lett. 105 (2010)

16 Hadron 2009 PACS-CS Collaboration, Phys.Rev.D79(2009) (2+1)-flavor, Wilson L =2.9 fm, a =0.09 fm m π (min) =156 MeV BMW Collaboration, Science 322 (2008) 1224 (2+1)-flavor, Wilson L =( ) fm, a =0.065, 0.085, fm m π (min) =190 MeV 3% accuracy of light hadron masses

17 Hadron 2011 Physical point simulations in (2+1)-flavor QCD PACS-CS Coll. (2010) X a=0.09 fm BMW Coll. (2011) a=0.054 fm a=0.065 fm a=0.077 fm a=0.093 fm a=0.116 fm X X X X 135 PACS-CS Coll.: Phys. Rev.D81 (2010) BMW Coll.: Phys. Lett. B701 (2011) 265

18 Toward large-scale Physical-point simulations 10PFlops K computer (RIKEN) First LQCD Simulation Now original plot by A. Ukawa

19 Advanced Institute for Computational Science (AICS) 10 Pflops supercomputer KEI 京 (full operation in 2012) Five strategic programs (FY ) 1. Life and Medicine 2. New Materials 3. Environment 4. Engineering 5. Particle, Nuclear and Astrophysics

20 Hot QCD LHC RHIC

21 Thermal QCD transition Order of QCD Transition Wuppertal-Budapest s LQCD EOS JHEP 1011 (2010) 77 2 nd order (u,d; m=0) 1 st order (u,d,s; m=0) crossover (real world) Critical Temperature Stefan-Boltzmann limit SB deff T T c : ~ 160 MeV ~ [K] Critical Energy Density ε c : ~ 2 GeV/fm 3 SPS@CERN RHIC@BNL LHC@CERN ~ 10 ε nm

22 Order of the QCD transition (T 0, μ=0) Finite size scaling 1/T L Budapest group, Nature 443 (2006) 675 Staggered, (2+1)-flavor, physical mass

23 Condensate fraction Pseudo-critical temperature HotQCD (HISQ/tree) Petreczky, HIS Wuppertal-Budapest (stout) JHEP 1009 (2010) 073 Fodor, Chiral susceptibility peak T pc = MeV

24 200 GeV/A PHOBOS 3 km BRAHMS PHENIX STAR LHC@CERN 5.6 TeV/A 27 km 5.5 TeV/A CMS LHC-B ALICE ATLAS X. N. Wang s talk

25 Dense QCD Sign problem (Complex Action)

26 Nuclear force: a brief history One-pion exchange Yukawa (1935) r Multi-pion Taketani et al. (1951) Repulsive core Jastrow (1951) Nambu (1957) repulsive core 2, 3,... EFT Weinberg (1990) high precision NN force (90 s-) parameters 5000 phase shift data

27 So I got up in the question period and I said, Maybe the reason is that inside the nuclear force of attraction, which holds nuclei together, there's a very strong short-range force of repulsion, like a little hard sphere inside this attractive Jell-O. I'll never forget, Oppenheimer got up, he liked to needle the young fellows and he said, very dryly, "Thank you so much for, we are grateful for every tiny scrap of help we can get. But I ignored his needle and pursued my idea, and actually calculated the scattering of neutrons by protons. I showed that it fit the data very well. Oppenheimer read my paper for the Physical Review and took back his criticisms. This work became a permanent element of the literature of physics.

28 E/A (MeV) Nuclear Force and EoS of Dense Matter Akmal, Pandharipande & Ravenhall, PRC58 ( 98) Phenomenological NN forces Neutron stars nuclei Z=0 N=Z ρ(fm -3 ) ρ 0 3ρ 0 5ρ 0 = 0.16 fm -3

29 Nuclear Force and Neutron Star NNN J (ρ max ~ 6ρ 0 ) PSR NN Oppenheimer-Volkov(1939) Pressure balance Fermi pressure Repulsive core gravity

30 Nuclear Force from Lattice QCD Univ. Tsukuba RIKEN Nihon Univ. Tokyo Inst. Tech. Univ. Tokyo S. Aoki, N. Ishii, H. Nemura, K. Sasaki K. Murano, T. Doi, T. Hatsuda T. Inoue Y. Ikeda B. Charron

31 How to define the NN potential from QCD? 1. NN wave function from lattice QCD 1. NN potential from the NN wave function 3. Derivative expansion LO LO NLO NNLO Ishii, Aoki, Hatsuda, Phys.Rev.Lett. 99 (2007) Ishii et al. (HAL QCD Coll.) Potential is a nice tool to calculate observables Potential is volume insensitive (=Lattice Friendly)

32 Key channels in NN scattering ( 2s+1 L J ) LO LO NLO NNLO 1 S 0 Central force nuclear BCS pairing Bohr, Mottelson & Pines, Phys. Rev. 110 (1958) 3 S 1-3 D 1 Tensor force deuteron binding Schwinger, Phys. Rev. 55 (1939), Bethe, ibid.57 (1940) Rarita & Schwinger, ibid. 59 (1941) 3 P 2-3 F 2 LS force neutron superfluidity in neutron stars Tamagaki, Prog. Theor. Phys. 44 (1970) Hoffberg et al., Phys. Rev. Lett. 24 (1970) Density profile of the deuteron with S z =±1 Pandharipande et al., (1998)

33 [Exercise 1] LO potentials : V C (r) & V T (r) quenched QCD quenched E ~ QCD 0 MeV E ~ 0 MeV quenched QCD E ~ 0 MeV Rapid quark-mass dependence of V T (r) Evidence of the one-pion-exchange Aoki, Ishii & Hatsuda, Prog. Theor. Phys. 123 (2010) 89

34 Central potential in (2+1)-flavor QCD HAL QCD Coll., in preparation 1 S 0 PACS-CS gauge config. (Clover + Iwasaki) a= 0.09 fm, L=2.9 fm m π = 700 MeV Physical point simulations (m π =135MeV with L=6fm & 9fm) will be carried out at KEI computer

35 Origin of the short range NN repulsion? Baryon-baryon force in flavor SU(3) x Six independent potentials in the flavor-basis Byproducts Hyperon forces : important for hyper-nuclei & neutron stars Fate of H-dibaryon: exotic 6-quark state (uuddss) Jaffe, PRL 38 ( 77)

36 c.f. Urbaryon models (Otsuku-Yasuno-Tamagaki 1965, Machida & Namiki 1965) Constituent quark model (Oka, Yazaki, Shimizu 1986) Lattice BB wave functions s Iwasaki + clover (CP-PACS/JLQCD config.) L=1.9 fm, a=0.12 fm, 16 3 x32 m π =835 MeV, m B =1752 MeV Inoue et al. (HAL QCD Coll.) Prog. Theor. Phys. 124 (2010) 591 Short range BB int. Quark Pauli principle 1 : allowed, 27 : partially blocked, 8 s : blocked

37 BB potentials in flavor-basis Inoue et al. [HAL QCD Coll.] Phys. Rev. Lett. 106 (2011) NPA (2012) to appear Repulsive core in NN channel Attractive core in H channel Growing NN tensor force

38 H-dibaryon from LQCD At physical point: M ΛΛ < M H < M ΞN? Inoue et al. [HAL QCD Coll.], NPA (2012) to appear exp. search at RHIC & J-PARC

39 Hypernuclei at J-PARC Japan(2009-) 3 known 40 known ~3000 known

40 BB potentials in flavor-basis Repulsive core in NN channel Inoue et al. [HAL QCD Coll.] Phys. Rev. Lett. 106 (2011) NPA (2012) to appear 1 S 0 channel 3 S 1 3 D 1 channel Attractive core in H channel Growing NN tensor force

41 NN phase shifts in the SU(3) symmetric world NN Stronger attraction in the deuteron channel Inoue et al. [HAL QCD Coll.] Phys. Rev. Lett. 106 (2011) NPA (2012) to appear

42 Simulating dense QCD by ultra-cold atoms

43 Ultra-cold atomic Gasses Figure from Pascal Naidon (RIKEN)

44 100 K 10 K 1 K 10-3 K 10-6 K 10-8 K

45 Universe 100 K 10 K 1 K 10-3 K 10-6 K 10-8 K

46 Universe 100 K 10 K 1K 10-3 K 10-6 K 10-8 K At these temperatures, quantum effects appear. Quantum motion is described by waves

47 Bose-Einstein Condensate 1995 Fermi superfluid K QUANTUM FLUIDS (SUPERFLUIDS) Universe 100 K 10 K Superfluid helium 1K 10-3 K 10-6 K atomic Condensation K At these temperatures, 1K quantum effects appear. Superconducting electrons 10 K Quantum motion is described by a single wave K Superfluid nucleons Superconducting quarks 109 K 1010K

48 Neutron Star Structure

49 Quark-Hadron transition in boson-fermion mixture of ultracold atoms Quark-Gluon Plasma qq qq Attractive Bose-Fermi Mixture Nuclear superfluid Fermion+Diquark Quark superfluid Induced superfluid Fermi-Bose mixture Maeda, Baym & Hatsuda, Phys. Rev. Lett. 103 ( 09)

50 Neutron Star Structure

51 π 0 and/or ρ 0 condensation in neutron matter A. B. Migdal, NPA (1972) Takatsuka, Tamagaki & Tatsumi, Prog. Theor. Phys. Suppl. 112 ( 83) 67 Kunihiro, Prog. Theor. Phys. 60 ( 78) 1229

52 Meson condensation in ultracold dipolar atoms Maeda, Hatsuda & Baym, in preparation. Sogo et al., NJP (2009) Fregoso & Fradkin, PRL 103 (2009)

53 Summary 1. New era of Latice QCD arrived massive physical point simulations will start from 2012 (u,d,s-flavor, L ~ 6fm, a ~ 0.05fm, m π =135MeV) 2. LQCD started to provide 1 st principle input for the physics of quark-gluon plasma EoS (P(T), ε(t)), spectral functions, etc RHIC, LHC 3. LQCD provides qualitative pictures on the NN, YN, YY & NNN forces better constraints of the EoS of dense matter physical point simulations will start from Ultracold atomic experiments may provide better understanding of the hadron-quark transition in dense matter

54 Future In a few years, we will hear more on 1. Physical point LQCD results for many observables 2. Simulations with better fermions staggered, Wilson domain wall, overlap 3. BB and BBB interactions better understanding of nuclei and neutron stars from QCD 4. UCA/QCD correspondence RHIC/LHC N obs. Lattice QCD AdS/CFT Ultracold atoms

55 END