Prospect of Experimental Nuclear Physics (in Japan) --Personal View-- Tohoku University H. Tamura Contents 1. Basic questions and present activities in nuclear physics 2. High-density cold matter 3. Hadrons in nuclei 4. Remarks 1. Basic questions and present activities in nuclear physics Big Bang Temp. (primordial universe) ? Quark Gluon Plasma (QGP) cooling by expansion Hadrons “gas” -> perfect liquid Baryons Mesons “liquid drop” ? Nucleo- systhesis superconductive ? Star Neutron star quark star? compression compression H, He→ Fe by gravity by gravity 0 Density Fe→ U Supernova? high density quark matter normal nucleus nuclear matter Big Bang Temp. (primordial universe) ? Quark Gluon Plasma (QGP) Puzzle of QGP coolingPuzzle by expansion of hadrons properties and (mass, confinement,Hadrons structure) phase diagram “gas” -> perfect liquid Baryons Mesons “liquid drop” ? Nucleo- systhesis superconductive ? Star Neutron star quark star? compression compression H, He→ Fe by gravity by gravity Puzzle of element 0 Puzzle of high density Density synthesis up to U cold matter Fe→ U Supernova? high density quark matter normal nucleus nuclear matter Big Bang Temp. (primordial universe) ? Quark Gluon Plasma (QGP)High energy HI collisions cooling by expansion （LHC, RHIC, GSI/FAIR） Hadrons “gas” -> perfect liquid Baryons Mesons Hadron physics （J-PARC, JLab, CERN,…） “liquid drop” ? Nucleo- systhesis superconductive Physics of Unstable Nuclei Neutron star ? Star（RIBF , GSI, MSU, GANIL,…） quark star? compression compression H, He→ Fe Presice Nuclear Physics by gravity by gravity （RCNP,…） Strangeness Density 0 Nuclear Physics Fe→ U Supernova? （J-PARC, JLab,…） high density quark matter normal nucleus nuclear matter “Prospects of Nuclear Physics in Japan” Feb. 2013 Nuclear Physics Executive Committee of Japan (312 pages, in Japanese) 1. Physics of Unstable Nuclei (RIBF,…) 2. Precise Nuclear Physics (RCNP,…) 3. Hypernuclei and Strangeness Nuclear Physics (J-PARC, JLab) 4. Hadron Physics (J-PARC, ELPH, RCNP-LEPS, CERN, JLab,…) 5. Physics of High Energy Heavy Ion Collisions (RHIC, LHC) 6. Nucleon Structure (RHIC, CERN, Femilab, J-PARC,…) 7. Fundamental Physics using Nuclear Techniques (J-PARC, RCNP, CERN, …) 8. Computational Nuclear Physics (Kei,…) 2. High Density Cold Matter Mistery of neutron star matter Highest density matter in the universe M = 1~2 M , R ~ 10~20 km => Density of the core = 3~10r （1～3 Btons/cm3） 0 Nuclear “Pasta” Various forms of matter made of almost only quarks Nuclear + Neutron Matter Neutron Matter L n Supefluid p n X Strange Hadronic Matter ? Quark Matter ?? High density nuclear Deconfined quarks matter with hyperons Color superconductivity (strange quarks) EOS (Equation Of State) for Nuclear Matter at T~0 Inner core (r > 2r0) Outer core (r < 2r0) How EOS changes Hyperon really appear? in n-rich matter? Density Fraction Which and how much? E = F( r, (nn,np,nY, …) ) ) Strange hadronic matter L Neutron-rich n n p nuclei (energy X Neutron matter E 2 r0 Hypernuclei r 0 r (density) Symmetric matter Ultra-cold Fermi gas p n Observation of Neutron stars Mass-Radius relation from pulsars Ordinary nucleus Cooling speed (nuclear saturation density: r ) 0 Gravitational waves from accretion Attractive LN interaction well established 89 39 LY49 -30 MeV L L’s potential depth = 30 MeV LN interaction is attractive (~2/3 of NN interaction) mL – mn = 180 MeV n Mass (-B :L binding energy) (MeV) L L weak int. n + n -> L + n L’s must appear at r = 2~3 r0 Hyperons mixing in the inner core outer core inner core assumptions - S N attractive (US = -15 MeV) - X N attractive (UX = -15 MeV) - S N repulsive (US= +30 MeV) Baryon fraction Baryon - X N attractive (UX = -15 MeV) L n p All the YN, YY interactions X Strange necessary ρ -> Understand Baryon-Baryon Ishizuka, Ohnish et al. hadronic matter Interactions in a unified way L LN int. in neutron matter? (effect by LN-SN force?) n-rich L hypernuclei LL int. looks weakly attractive. To be established. XN int. unknown (attractive??) LL hypernuclei X hypernuclei Mystery in EOS Hyperons must appear at r = 2~3 r0 EOS with hyperons (or kaons) too soft -> too high density -> easily form a BH and cannot support 1.97±0.042 Msun NS A big mistery in nuclear physics Unknown repulsion at high r Framework should be reconsidered Strong repulsion in three-body force (NNN, YNN, YYN, YYY) Demorest et al., Nature 467 (2010) 1081 Change of meson-baryon coupling constants or baryon structure Phase transition to quark matter (quark star or hybrid star) M Quark Meson Coupling model with hyperons Hyperons NS mass J.Stone et al., Nucl. Phys. A792(2007)341 Quark matter NS radius (km) No direct measurement An important direction: “Hadrons in Nuclei” Properties of mesons in nuclei Vector meson mass in a nucleus (pA collision) K- nucleus, p nucleus, h’ nucleus bound states Properties of hyperons in nuclei mL in hypernuclei Single particle energies and weak decay properties of L in hypernuclei NN Short Range Correlations Role of tensor force in nuclear structure DIS and the EMC effect => Clues to understand high density cold matter 3.1 Hadrons in Nuclei -- Vector meson mass in nuclei Origin of hadron mass Experimental evidence of hadron mass generation by chiral symmetry breaking? -- Effective (u,d) quark mass should be partially restored in nuclear matter density To be observed as hadron mass change in nuclei. Implications from e+e- invariant mass spectra in HI collisions Mass shift of f -> e+e- in pA reaction (KEK E325) e- e- e+ e+ + - w → e e f -> e+e- Cu bg <1.25 Cu PRL96(06)092301 PRL98(07)042501 Mass of vector mesons in nucleus J-PARC E16 x100 statistics of KEK E325 Dispersion relation (dependence on b) Dependence on nuclear density -> Detailed comparison with QCD Chiral Chiral Spectrometer Spectro- meter EM calorimeter Nuclear Target 30/50 GeV primary beam Cherenkov GEM Tracker 5m J-PARC E16 x100 statistics of KEK E325 Dispersion relation (dependence on b) Dependence on nuclear density -> Detailed comparison with QCD Chiral Chiral Spectrometer Spectro- meter EM calorimeter Nuclear Target 30/50 GeV primary beam Cherenkov GEM Tracker 5m 3.2 Hadrons in Nuclei -- K- bound states Very dense matter? K--nucleus bound states Strong K-p attraction from K- p atomic/scattering data Under a big debate by theorists: Deep (150~200 MeV, phem. models) or shallow (~50 MeV chiral model)? Experimental hints of K- nuclei But still controversial K- can make a nucleus extremely dense. –> The only experimental method to produce cold and dense matter. - K may condensate in n-star at high r - - 11 InvariantStopped KMass- on 6,7 ofLi, K12Cpp Missing Mass of K C Back-to-back L-p pair density BK ~ -115 MeV p Re(V) ~ -180 MeV p K- M. Agnello et al., PRL 94 (2005) 212303. Dote et al. PLB590 (2004) 51 T. Kishimoto et al., PTP 118 (2007) 181 - J-PARC E15 for “K-pp” Slide from J-PARC E15 p p K- K-pp bound state Theoretical estimate for K- 3He -> “K-pp” + n T. Hashimoto (E15) INPC2013 3.3 Hadrons in Nuclei -- L’s magnetic moment in a nucleus Magnetic moment of L in a nucleus Constituent quark model works well for baryon m. Partial restoration of chiral symmetry affects baryon m ? mL e h m = m : Const. quark mass q 2m c q q mq decreases in a nucleus -> m increases? -> What is a constituent quark ? What is the origin of the baryon spin? L in 0s orbit is the best probe gc gL ψL↑ψc B(M1) of L-spin-flip M1 transition Jc +1/2 Jc M1 in s-orbit "hypernuclear fine structure" Jc -1/2 core nucleus ψL↓ψc L in s-orbit hypernucleus g is assumed to be unchanged by a L Doppler Shift c ~100% Attenuation Method L-spin-dependent LN interaction is small LN spin-spin force ~ 1/10 of NN spin-isospin force LN spin-orbit force ~ 1/40 of NN spin-orbit force Change of nucleon m in a nucleus? mN 8±3% enhanced after removing the effect of meson exchange current. 7 Preliminary data on gL in LLi (BNL E930) 10 - - 10 10 + 7 + 3 B (K , p ) LB*, LB*(3 ) -> LLi*(3/2 ) + He indirect population simulation + 3+ 7/2 preliminary + +0.4 5/2 - gL = 1.1 - 0.6 mN (statistical error only) + First data of g in nucleus 3/2 L + - gL(free) = 1.226 mN 1 + 6Li 1/2 7 Li L 7 J-PARC E13 Precise(~3%) measurement of |gL-gc| for LLi X hypernuclei LL hypernuclei Hadron Hall and X-atomic X rays Hypernuclear weak decays L hypernuclearapproved/proposed g spectroscopy Pion double chargeexperiments exch. reaction n-rich L hypernuclei w mesonic nucleus Pentaquark Q+ search Sp scattering - K pp bound state search H dibaryon search Beam Dump K1.8 Hadron mass in nuclei Quark structure of nucleon Spectroscopy of charmed baryons 0 K L rare decays K1.8BR KL K-pp bound states K- atomic X rays Production K1.1 high mom. line L(1405) properties target (T1) h mesonic nuclei K1.1BR -> Funded T violation in K+ decays f mesonic nucleus Lepton universality in K+ decays L hypernuclear g spectroscopy Confirmation of pentaquark Q+ S nuclear systems 30~50 GeV YN scattering primary beam Q+ hypernuclei Approved(stage-2) / Approved(stage-1) / proposed or LOI m-e conversion 3.4 Hadrons in Nuclei -- NN Short Range Correlations and the EMC effect DIS for NN and NNN in Short Range Correlation Nucleon swelling? 12C(e,e’pn), (e,e’pp), (e,e’nn) Correlated NNN CLAS collaboration, PRL 96, 082501 (2006) Correlated NN Relation between EMC effect and SRC L. B. Weinstein et al., PRL 106 (2011) 052301 CERN Courier, May 2013 80% 20% Previously, EMC effect (at large x) was interpreted as nucleon swelling (partial deconfinement), but Nucleons look “modified” only when they are interacting at a close distance? EMC effect seems nothing to do with partial deconfinement or partial restoration of chiral symmetry, but is it true? SRC and EMC effect provide information on what’s happening in high-density cold matter.