“Summary” -- Personal comments and personal answers to the PAC requirements--
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Transcript of “Summary” -- Personal comments and personal answers to the PAC requirements--
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“Summary”-- Personal comments and
personal answers to the PAC requirements--
Dept. of Physics, Tohoku UniversityH. Tamura
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1. What is necessary to understand of the elementary process of electro-production of strangeness2. Experimental study of light hypernuclei and YN interaction including Charge Symmetry Breaking (CSB) effect and N-N coupling.3. What can be learned from precise determination of binding energies4. Deformation of core-nucleus and energy levels of hypernuclei5. Detailed spectroscopy of heavy hypernuclei and potential impacts of measurement to mean-field theory, shell-models and single particle nature of in deep inside of nuclei.6. Uniqueness of JLab hypernuclear program in contrast to other facilities such as J-PARC, Mainz, future FAIR
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Contents
1. Elementary Process
2. N interaction from light hypernuclei
--- Charge Symmetry Breaking
3. Impurity effects
4. Single Particle Energies of hypernuclei
5. Uniqueness of JLab
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Motivations of strangeness nuclear physics
BB interactionsUnified understanding of BB forces by u,d ->u, d, s
particularly short-range forces by quark pictures Test lattice QCD calculations
Properties and behavior of baryons
in nucleiin a nucleus,
Single particle levels of heavy hypernuclei
...
Impurity effectin nuclear structure Changes of size,
deformation, clustering, Appearing new symmetry,
…
Clues to understandhadrons and nuclei
from quarks
Cold and dense nuclear matter
with strangeness
What can JLab answer?
Charge Symmetry Breaking
New means to clearly probe the exotic nuclear
structure(e.g. triaxial deformation)
Study of high-density(strange) nuclear
matter from s.p.e. of heavy hypernuclei
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2. Elementary Process Markowitz, Bydzovsky, Carman
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CLAS: Wonderful data for cross sections and all combinations of beam, target, andrecoil polarization states.- Precision data – broad kinematic coverage- Program includes “complete” experiments on both proton and neutron targetsCLAS data dominates the world’s strangeness physics database for both photoandelectroproduction cross sections and spin observables.lso essential data for photoproduction models
Carman
CLAS data are wonderful, but very forward angles are not covered.
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Markowitz
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Markowitz
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The largest merit of (e,eK+) is the accuracy of absolute energy (<100 keV), butwith demerits of non-selectivity of states and difficulty in state assignment.
The cross section is the almost only observablethat can be used for state assignment.
For this purpose, reliable theoretical calc’s of the cross sections are essential, and therefore the elementary cross section must be precisely known.Target thickness should be carefully monitored: -> The waterfall target looks good.
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Hashimoto and Tamura, PPNP (2005)Calc. by Motoba and Itonaga
(+,K+) cross sections well reproducedby DWIA calc.
Why not in (e,e’K+)with much less distortion?
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Also essential data for photoproduction models
Bydzovsky
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3. N interaction
from light hypernuclei
--Charge Symmetry Breaking
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N interaction has been rather well known throughinterplay between Theories of BB models (Haidenbauer, Rijken) and Theories of hypernuclear structure (Millener, Hiyama, Motoba, Wirth) with Good experimental data from Hall A (Urciuoli), Hall C (Nakamura) KEK/BNL/J-PARC (Tamura), FINUDA (Bressani) except for CSB problem -> A big surprise? (Hiyama, Gibson)
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Millener
Spin-dependent force strengthswell determined from p-shellLevel structures-> feedback to BB int. models
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Wirth
Ab-initio calculation of p-shell hypernuclei w/ mixing is now on-going! –Stringent test of YN interactions
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Charge symmetry breaking Exp: Achenbach, Urciuoli, Nakamura, Tamura, Tang,
Theor: Millener, Hiyama, Haidenbauer, Nogga, Gibson, Motoba
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3He+Λ0 MeV
-2.390.03
1+
0+
3H+Λ0 MeV
-2.040.04
1+
0+
n n
p Λ
4HΛ4HeΛ
n
p Λ
p
ΔB (He-H) = 0.350.06
The The AA = 4 isospin doublet = 4 isospin doublet
ΔB (He-H) = 0.24-1.24
-1.00
Nucleon-hyperon interaction can be studied by strange mirror pairs Coulomb corrections are < 50 keV for the 4
ΛH - 4ΛHe pair
Energy differences of 4ΛH - 4
ΛHe pair much > than for 3H - 3He pair
Achenbach
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Nakamura
Systematic error of absolute energy ~100 keV!
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Nakamura
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Fit 4 regions with 4 Voigt functionsc2
/ndf = 1.19
Binding Energy BL=13.76±0.16 MeVMeasured for the first time with this level of accuracy (ambiguous interpretation from emulsion data; interaction involving L production on n more difficult to normalize)
Within errors, the binding energy and the excited levels of the mirror hypernuclei 16O and 16N (this experiment) are in agreement, giving no strong evidence of charge-dependent effects
Results on 16O target – Hypernuclear Spectrum of 16N
Urciuoli
There seems to be little CSB effects for A>4.
Reliable data for A=4 should be measured.
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3He+Λ0 MeV
-2.390.03
1+
0+
3H+Λ0 MeV
-2.040.04
1+
0+
n n
p Λ
4HΛ4HeΛ
n
p Λ
p
ΔB (He-H) = 0.350.06
The The AA = 4 isospin doublet = 4 isospin doublet
ΔB (He-H) = 0.24-1.24
-1.00
Nucleon-hyperon interaction can be studied by strange mirror pairs Coulomb corrections are < 50 keV for the 4
ΛH - 4ΛHe pair
Energy differences of 4ΛH - 4
ΛHe pair much > than for 3H - 3He pair
Suspicious.Measure at J-PARC Tamura
-ray
4He + -
Pion decayspectorscopy
4He(e,e’K+)spectorscopy
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Pion decay spectroscopy A powerful tool particularly for CSB
Achenbach, Tang, Motoba
Proposing Setup at JLab 12
Tang
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Hyperhydrogen peak searchHyperhydrogen peak search
Emulsion data
MAMI data
local excess observed inside the hyperhydrogen search region
preliminary
Achenbach
Sys. Error: ± 110 (calib.) ± 40 (stab.) keV/c
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World data on World data on A = 4A = 4 system system Achenbach
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Gibson
Proposed to measure a(n)by K-
stop d -> n
-> at J-PARC
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Motoba
4He(e,e’K+)spectorscopy
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Haidenbauer, Nogga
What is the origin of CSB ?Construct YN interaction
from chiral EFT-> applied to CSB problem
Admixture from couplingdetermines CSB effect
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4. Impurity effects Hiyama, Isaka, Nakamura
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single particle energy
GSND SD
41Ca
40Ca(Pos)⊗(s)
40Ca(Pos)⊗(s)
40Ca(Pos)GS
NDSD
40Ca
Energy surface
spherical
41Ca
spherical
superdeformed
superdeformed
39Ar
: linear relation
IsakaB is a measure of deformation
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5/2
1/2+
3/2-
α + α +n α + α +n+ Λ
-10.52 MeV
-8.14
-7.35
-1.58
+0.1
+0.6 MeV
MeV
BΛ
= 8.94 MeV
CA
L
( B
Λ = 9.11 0.22 M
eV)
EX
P
10BeΛ
9Be
Level reversion is occurred
by addition of a Λ particle.
10B(e,e’K+)10Be
(Jlab E01-11)
ND
ND
SD
1-, 2-
2-, 3-
0+ , 1+
Small spin-splitting is
neglected to show.
Λ
If we observepositive states andnegative states,we find thatΛ-separationenergies are dependenton the degree ofdeformation.Please observe the positive parity states at Jlab.
10BeΛHiyama
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If 24Mg is triaxially deformed nuclei
Large overlap leads to deep binding
Middle
Small overlap leads to shallow binding
Triaxial deformation
Prolate deformation
G.S.
Exci
tatio
n En
ergy
25Mg
24Mg⊗s-orbit)
24Mg⊗p-orbit)
Split into 3 states?
p-states split into 3 different state
Observing the 3 different p-states is strong evidence of triaxial deformationOur (first) task: To predict the level structure of the p-states in 25
Mg
IsakaTriaxial deformation
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Results: Excitation spectra– 3 bands are obtained by hyperon in p-orbit
• 24Mg⊗p(lowest), 24Mg⊗p(2nd lowest), 24Mg⊗p(3rd lowest)
Lowest threshold : in between 8.3 and 12.5 MeVNe +
21
Splitting of the p states
Isaka
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Distinguish Normal Deformed / Super Deformed states 10
Be <= 10B(e,e’K+) : level inversion Probably (spin)-parity cannot be assigned. Hopefully distinguished from cross sections. But how small ? Evidence for triaxial deformation (there are implications
but no clear evidence.) 27
Mg <= 27Al (e,e’K+) Three band heads should have large cross sections.
Impurity - changes the size/deformation of the core nucleus ? => Only for light-clusterized nuclei (7
Li 19% shrinkage from 6Li: Tanida et al.) - is a clear probe of nuclear shape/nuclear density.
“New means to measure nuclear structure”
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5. Single Particle Energies
of hypernuclei
( and neutron star matter)
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Nakamura
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Millener
Now, we can make this plot with ~100 keV accuracy of absolute energy.
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Galibaldi
How??How??
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Hyperons must appear at = 2~3 0
EOS’s with hyperons (or kaons) too soft -> can support M < 1.5 Msun
M
NS radius (km)
NS
mas
s
Unknown repulsion at high Strong repulsion in three-body force including hyperons are necessary. (NNN, YNN, YYN, YYY)
Phase transition to quark matter ? (quark star or hybrid star)
But we have no data on BBB force at highnuclear matter, except for indirect info. in HI collisions.
Serious problem in the nuclear physics at present
Quark matter
Hyperons
PSR J0348-0432 (2013) 2.01±0.04 Msun
“The heavy neutron star puzzle”
PSR J1614-2230 (2010) 1.97±0.04 Msun
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Vidana
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Vidana
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TBF repulsion from meson exchange models is not enough
Vidana
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’s single particle energy in hypernuclei will solve this serious problem?
Nijmegen ESC08 reproduces (almost) all the hypernuclear data as well as all the NN/YN scattering data.
Y. Yamamoto/RijkenBHF calc. from ESC08 => reproduces all the s.p.e. data (~1 MeV accuracy) very well with no adjustable parameters => but EOS is too soft.ESC08 + “3body/4body repulsion in YNN,YYN,YYY..” with the same size as the NNN repulsion which reproduces HI collision data (“universal 3B repulsion”). => can support 2Msun NS. => slight change of Bby +- 0.5 MeV between A~30 and 208.
Rijken
Even with nuclei, we can see the effect of a (short-range) 3-body YNN/YYN/YYY repulsion in B, if the repulsion is large enough to support 2Msun NS.
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Y. Yamamoto
+ 3B/4B repulsion in NNN +YNN
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EOS and NS mass
ESC08 only ESC08 only
+ 3B/4B repulsion in NNN only
+ 3B/4B repulsion in NNN +YNN
+ 3B/4B repulsion in NNN +YNN
+ 3B/4B repulsion in NNN
Rijken/Yamamoto
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We need accurate (< 0.1 MeV) B data for at least three hypernuclei,
a heavy (A~200), a medium-heavy (A~100-50), and medium (A~30)
208 Pb is quite important, as far as experimentally feasible.
Theoretical efforts are also important: Include relativistic effects Physical picture of 3B/4B forces -- 3B force from lattice??
hyperon in the only probe that can sense static high-density (but, up to ~) nuclear matter.
( HI collisions are not static and difficult to treat.)
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Slope: [B(A’)-B(A)]/(A’-A)
Is there a correlation between the slope in B(A) plot and the NS maximum massIndependently of theoretical treatment ??
NS
max
imum
mas
s
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Motoba
From such calculation, we can separate excited hole states and extract the g.s. energy reliably.
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Pederiva, LonardoniQuantum Monte Carlo for hypermatter with 3B force
BenharSpectral function of in 208Pb
DragoNeutron star with hyperons, and quark-hybrid star
SchulzeNeutron star with hyperons from BHF + SHF
MotobaPionic weak decays of hypernuclei
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6. Uniqueness of JLab
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Uniqueness of JLab(1) Absolute mass in ~100 keV accuracy with HKS (a wide acceptance both for and 0) Nakamura (HRS needed a slight correction in B ) Urciolli
c.f. (,K+) and (K-,) reactions (n->) have no means for absolute calibration. Affected by emulsion data. (,K+) error in B: typ. ~0.5 MeV(thick target) + emulsion error
0.5 MeV should be shifted in all the (,K+) Bvalues. Millener
Confirmed from the accurate (e,e’K+) data
-> Definite data for CSB from light hypernuclei-> ’s s.p.e. in medium/heavy hypernuclei
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(2) High resolution from a high-quality / intense beam (and a thin target)-> Highest resolution in reaction spectroscopy ~ 500 keV (FWHM) -> High accuracy in decay pion (< 100 keV) separate core levels (different hole states), SCB in light systems
Complementary to -spectroscopy:Eex =2—10 keVOnly bound statesOnly excitation energy (not absolute mass) -- Absolute value of the g.s. mass is necessary for physics of CSB, impurity, and s.p.e.
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K10
HR
KL
K1.1
K1.8
K1.8BR
High-p
KL
Hadron HallExtension Plan
COMET
K1.1BR/K1.1
CharmS=-3systems
PreciseS=-1systems
S=-1 systems
S=-2 systems
2nd production target
3rd production
target
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K10
HR
KL
K1.1
K1.8
K1.8BR
High-p
KL
Hadron HallExtension Plan
COMET
K1.1BR/K1.1
CharmS=-3systems
PreciseS=-1systems
S=-1 systems
S=-2 systems and hypernucleiatoms, YN scattering
H dibaryon
K-pp systems, K atoms, (1405), nucleus
*, * spectroscopyinteractions
hypernucleiMulti K mesons in nuclei
Charmonium Spectroscopy Charmonium and D mesons in nuclei
2nd production target
3rd production
target
Single particle energies of n-rich hypernuclei
Magnetic moments of hypernuclei Weak decays of hypernuclei
Hadron mass in nucleiNucleon structure (Drell-Yan)
Charmed baryons
-spectroscopy and weak decays of hypernuclei
nuclear systemsYN scattering
nucleus bound states
Precise S= -1 exp.
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HIHR LineJ-PARC ExHH
A23
ElectrostaticSeparator
Prod. T
Dispersive Beam
High Res.Spectrometer
Exp. Target
Mass Slit
AchromaticFocus
Intensity: ~ 9x108 pion/pulse (1.2 GeV/c, 56 m, 1msr*%, 270kW, 6s spill, Ni 54mm)p/p ~ 1/10000
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Precise single particle energies from (,K)
E ~ 200 keV (FWHM)Problem:Absolute energy calibration impossibleHuge cost of the new hall and HIHR line
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JLab: High resolution/high accuracy S=-1 spectroscopy Pi decay spectroscopy
Mainz: Elementary process, … Pi decay spectroscopy
J-PARC: S= -2 systems S=-1 -spectroscopy K- and other mesons in nuclei
FAIR: HI induced (n-righ/p-rich) hypernuclei S=-2 -spectroscopy Anti-hyperon in nuclei
Pochodzalla
Tamura
Comparison
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Summary of summary
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Motivations of strangeness nuclear physics
BB interactionsUnified understanding of BB forces by u,d ->u, d, s
particularly short-range forces by quark pictures Test lattice QCD calculations
Properties and behavior of baryons
in nucleiin a nucleus,
Single particle levels of heavy hypernuclei
...
Impurity effectin nuclear structure Changes of size,
deformation, clustering, Appearing new symmetry,
…
Clues to understandhadrons and nuclei
from quarks
Cold and dense nuclear matter
with strangeness
What can JLab answer?My personal idea
Charge Symmetry Breaking4H pi decay, 4
H* production,..
New means to clearly probe the exotic nuclear
structure(e.g. triaxial deformation)
Study of high-density(strange) nuclear
matter from s.p.e. of heavy hypernuclei
e.g. 208Pb, A=50~100,
27Mg
Elementary H(e,e’K+)
27Mg
Needs more theoretical studies
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Backup
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First determination of p for 8 Hypernuclei (cont’d)
K. Itonaga, T. Motoba, Progr. Theor. Phys. Suppl. 185 (2010) 252. K. Itonaga, T. Motoba, Progr. Theor. Phys. Suppl. 185 (2010) 252.
H. Bhang et al., JKPS 59 (2011) 1461. H. Bhang et al., JKPS 59 (2011) 1461.
J.J. Szymansky et al., PRC 43 (1991) 849.J.J. Szymansky et al., PRC 43 (1991) 849. H. Noumi et al., PRC 534 (1995) 2936. H. Noumi et al., PRC 534 (1995) 2936.
M. Agnello et al., PLB 681 (2009) 139. M. Agnello et al., PLB 681 (2009) 139.
K. Itonaga, T. Motoba, Progr. Theor. Phys. Suppl. 185 (2010) 252. K. Itonaga, T. Motoba, Progr. Theor. Phys. Suppl. 185 (2010) 252.
H. Bhang et al., JKPS 59 (2011) 1461. H. Bhang et al., JKPS 59 (2011) 1461.
J.J. Szymansky et al., PRC 43 (1991) 849.J.J. Szymansky et al., PRC 43 (1991) 849. H. Noumi et al., PRC 534 (1995) 2936. H. Noumi et al., PRC 534 (1995) 2936.
T. Motoba et al., NPA 534 (1991) 597. T. Motoba et al., NPA 534 (1991) 597.
A. Gal, NPA 828 (2009) 72. A. Gal, NPA 828 (2009) 72.
T. Motoba, K. Itonaga, Progr. Theor. Phys. Suppl. 117 (1994) 477. T. Motoba, K. Itonaga, Progr. Theor. Phys. Suppl. 117 (1994) 477.
M. Agnello et al., PLB 681 (2009) 139. M. Agnello et al., PLB 681 (2009) 139.
K. Itonaga, T. Motoba, Progr. Theor. Phys. Suppl. 185 (2010) 252. K. Itonaga, T. Motoba, Progr. Theor. Phys. Suppl. 185 (2010) 252.
H. Bhang et al., JKPS 59 (2011) 1461. H. Bhang et al., JKPS 59 (2011) 1461.
J.J. Szymansky et al., PRC 43 (1991) 849.J.J. Szymansky et al., PRC 43 (1991) 849. H. Noumi et al., PRC 534 (1995) 2936. H. Noumi et al., PRC 534 (1995) 2936.
New results from FINUDA Bressani
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◆ n-rich hypernuclei by (-,K+)
◆ spectroscopy of hypernuclei -> N, N-N (NN) int.
◆ K-pp by 3He(K-,n) ◆ K-pp by d(+,K+)
-> KbarN int. in matter => K condensation in n star?◆ p scattering -> n ( p) (Quark Pauli effect) , p->N int.
E10
E15
E40
E13
frac
tio
n
ρ
nn attractive
K-
pp
=> Fraction of in n-rich matter
E27
=> exists in n-star?
Under preparationReady to runPartly took data
◆ hypernuclei -> interaction , correlation?
◆ hypernuclear spectroscopy ◆ atomic X rays -> N interaction
◆ H dibaryon search from H->, p -> Short-range BB force (Color magnetic int.)
E05 E03, E07
E42
=> fraction in Strange Hadronic Matter
=> exists in n-star?
E07
Status of Strangeness NP @J-PARC
Property of high density nuclear systems
SHM
TamuraStatus of J-PARC
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Nakamura
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Rijken