“Summary”-- Personal comments and

personal answers to the PAC requirements--

Dept. of Physics, Tohoku UniversityH. Tamura

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

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

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

2. Elementary Process Markowitz, Bydzovsky, Carman

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.

Markowitz

Markowitz

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.

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?

Also essential data for photoproduction models

Bydzovsky

3. N interaction

from light hypernuclei

--Charge Symmetry Breaking

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)

Millener

Spin-dependent force strengthswell determined from p-shellLevel structures-> feedback to BB int. models

Wirth

Ab-initio calculation of p-shell hypernuclei w/ mixing is now on-going! –Stringent test of YN interactions

Charge symmetry breaking Exp: Achenbach, Urciuoli, Nakamura, Tamura, Tang,

Theor: Millener, Hiyama, Haidenbauer, Nogga, Gibson, Motoba

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

Nakamura

Systematic error of absolute energy ~100 keV!

Nakamura

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.

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

Pion decay spectroscopy A powerful tool particularly for CSB

Achenbach, Tang, Motoba

Proposing Setup at JLab 12

Tang

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

World data on World data on A = 4A = 4 system system Achenbach

Gibson

Proposed to measure a(n)by K-

stop d -> n

-> at J-PARC

Motoba

4He(e,e’K+)spectorscopy

Haidenbauer, Nogga

What is the origin of CSB ?Construct YN interaction

from chiral EFT-> applied to CSB problem

Admixture from couplingdetermines CSB effect

4. Impurity effects Hiyama, Isaka, Nakamura

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

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

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

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

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”

5. Single Particle Energies

of hypernuclei

( and neutron star matter)

Nakamura

Millener

Now, we can make this plot with ~100 keV accuracy of absolute energy.

Galibaldi

How??How??

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

Vidana

Vidana

TBF repulsion from meson exchange models is not enough

Vidana

’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.

Y. Yamamoto

+ 3B/4B repulsion in NNN +YNN

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

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.)

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

Motoba

From such calculation, we can separate excited hole states and extract the g.s. energy reliably.

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

6. Uniqueness of JLab

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

(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.

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

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.

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

Precise single particle energies from (,K)

E ~ 200 keV (FWHM)Problem:Absolute energy calibration impossibleHuge cost of the new hall and HIHR line

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

Summary of summary

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

Backup

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

◆ 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

Nakamura

Rijken