Satoshi N Nakamura - Jefferson Lab€¦ · Oct. 25th 2007 S N Nakamura for HKS/HES collaboration...
Transcript of Satoshi N Nakamura - Jefferson Lab€¦ · Oct. 25th 2007 S N Nakamura for HKS/HES collaboration...
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Satoshi N NakamuraTohoku UniversityHUGS 2010 Lecture14 -17 June 2010 @ Jefferson Lab
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Introduction
Nuclear physics in a nutshell
Brief history of hypernuclear study
(p,K) reaction hypernuclear spectroscopy
(e,e’K) reaction hypernuclear spectroscopy
Decay-g, p hypernuclear spectroscopy
Other hypernuclear studies & Future experiments
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Interaction Classical Theory (Macroscopic)
Field Theory(Microscopic)
Gravity
Electromagnetic
Weak
Strong
14 Jun 2010 S N Nakamura @ Tohoku Univ.
PlanetsStars
Almost all phenomena around us
Beta-decay of nuclei
Nuclear Force
Difficult to Solve
General Relativity
Electrodynamics
Quantum Gravity
Quantum Electrodynamics
(QED)
Electro-weak (Weinberg-Salam-
Grashow)
QuantumChromodynamics
(QCD)
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14 June 2010 S N Nakamura @ Tohoku Univ.
Material Physics (Many body Problem)
Particle Physics(Single body Problem)
Observational Cosmology
NuclearPhysics
(Few body Problem)
Gravity
EM
Weak
Strong
1 1024
10 102 103
1m
1016m
10-15m
Deg. Of Freedom
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14 June 2010 S N Nakamura @ Tohoku Univ.
down
up
strange
charm top
bottom
2.6
4.9
~1270
104 ~4200
~170000
Stable unstable(life ~10-10 s)
Mass(MeV/c2)
23
e+
13- e
Very unstable(life <10-12 s)
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Up (3MeV/c2)+ Up (3MeV/c2)
+ Down (5 MeV/c2)
11MeV/c2
Proton Mass938.272 MeV/c2
Why is heavier system more stable?What is the source of >95% of mass?
Higgs Mechanism
Chiral symmetry breaking
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14 June 2010 S N Nakamura @ Tohoku Univ.
L Strange Quark
Up Quark
Down Quark
Hyper NucleusProton
Neutron
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N
Z L, S hypernuclei39 L1 S
Nu ~ Nd ~ Ns
Higher density
stra
ng
en
ess
0
1
2
stableunstable
LL, X hypernuclei3 LL
Courtesy of M.Kaneta, H.Tamura
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Updated from: O. Hashimoto and H. Tamura, Prog. Part. Nucl. Phys. 57 (2006) 564.
(2009)
52LV
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14 June 2010 S N Nakamura @ Tohoku Univ.
Nuclear Force (NN) Baryon Force (YN,YY)
Nuclear Matter Baryon Matter(Neutron, Hyperon, Quark Stars)
Nuclear Structure Modified by impurity(Size, shape, symmetry…)
Baryon weak int.study is difficult
Hyperon weak decay and medium effect
n p
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Oct. 25th 2007 S N Nakamura for HKS/HES collaboration
Nuclear Force (NN) Baryon Force (YN,YY)
Nuclear Matter Baryon Matter(Neutron, Hyperon, Quark Stars)
Nuclear Structure Modified by impurity(Size, shape, symmetry…)
Baryon weak int.study is difficult
Hyperon weak decay and medium effect
NASACygnus X-3
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Oct. 25th 2007 S N Nakamura for HKS/HES collaboration
Nuclear Force (NN) Baryon Force (YN,YY)
Nuclear Matter Baryon Matter(Neutron, Hyperon, Quark Stars)
Nuclear Structure Modified by impurity(Size, shape, symmetry…)
Baryon weak int.study is difficult
Hyperon weak decay and medium effect
eg.) 7LLi Shrinkage
6Li 7LLi
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Oct. 25th 2007 S N Nakamura for HKS/HES collaboration
Nuclear Force (NN) Baryon Force (YN,YY)
Nuclear Matter Baryon Matter(Neutron, Hyperon, Quark Stars)
Nuclear Structure Modified by impurity(Size, shape, symmetry…)
Baryon weak int.study is difficult
Hyperon weak decay and medium effect
Lifetime of hypernuclei
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cbabcaaa
a
a
j
a
iji
a
iiQCD
GGgfGGG
GGqTqgGqmiq
gg
4
1)(L
gg
AAF
FFAemiQED
4
1)(L
Non perturbative theory : gluon has color
Perturbative theory : photon has no charge)10(0360003.137
4)0(
12
1
p
ea
1~4
)0(
12
1
p
gas
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(g-2)electron = 1 159 652 175.86 (0.10)(0.26)(8.48 )x 10-12
Errors (a4)(a5)(a1 input)
891 Feynman diagrams, 7 ppb accuracy
(g-2)electron PDG = 1 159 652 181.1(0.7) x 10-12
Kinoshita & Nio, PRD 73 013003 (2006)
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3-JETs rate from e+ e- annihilationBethke, Physics B 54A (1997) 314
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L
L
L...
))/ln(
))/ln(ln(21
)/ln(
4~)(
2
2
20
1
2
0
pa s
L : Cut off 100 – 400 MeV
s quark mass ~100MeV
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10 MeV 100 MeV 1GeV
QCDL QCDNuclear Force
10 fm 1 fm 0.1 fm
fmMeV197~~ cEx
R(p)~0.8fm
R(12C)~2.6fmR(208Pb) ~6.6fm
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Mass, Spin, Lifetime, Parity, ….
Interaction
World is not so simple ….
Can simple extension handle manybody problems ?
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Principle of Superposition?
3-body force?
Even in Newton Mechanics :3-body problem cannot be exactly solved in general.
Approximation / Model
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>1023 lnbkS
\
i
i
NNN
xHxxH
xHxxxHxxxH
)(,...),(
)(),...,,(),...,,(
21
12121
Statistical approach may apply.
Mean field approach
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1 2 10 100 1023
Elementary
Bare interaction
Manybody
Statistical Approach
Fewbody
Nuclear Physics = Strong Interaction+ Fewbody problem
Mean Field Approach
(my definition)
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20 MeV 200 MeV 2GeV
QCDL QCD
Meson Exchange
Nuclear Force Model
QCD inspired modelsChiral perturbation
Effective Field TheoriesQuark Meson Coupling
10 fm 1 fm 0.1 fm
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QCD cannot be simply applied to describe NFin low energy
Phenomenological interaction model between nucleons.
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Each particle’s sizeInteraction
Known (measurable)
Cluster may be analyzed
Size of a bag which contains iron sandWill you analyze the motion of bag
from interaction & geometry of particles?
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Nucleus is most dense material in the world.
But, nucleon moves almost freely : Fermi Gas
Is nuclear force weak!?
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B/A ~ 8MeV for all nuclei (A>30)
B = Zmp + (A-Z)mn – m(AZ)
Z : atomic number (number of protons)A : Mass number (number of nucleons)
5626Fe, 62
28Ni
Number of nucleons for a nucleon to interact with is almost the same.
Interaction length of nuclear force is smallNucleon density in nucleus is constant r ~ 0.17/fm3
(otherwise B/A depends on nuclear size)
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M(A,Z) = Z mp + N Mn nucleon mass
– avA volume term
+as A2/3 surface term
+ac Z2/A1/3 Coulomb term
+aa (N-Z)2/4A asymmetric E
+d(A,Z)A-1/2 pairing interaction
Except for Coulomb term, symmetric for (Z,N)
Charge Symmetry of Nuclear Force
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(Proton = Neutron) for nuclear force
Charge symmetry of nuclear force
Consider p, n as the different internal quantum states of the same particle (nucleon).
IsospinSU(2) symmetry
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r ~ 0.17/fm3 ~ 3 x 108 ton/cm3
Electric force e2/(1fm)2~230N~23.5kgw
Nuclear force is attractive enough to bind Coulomb repulsive protons.
Nuclear force should be repulsiveso that nucleus does not collapse.
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High statistics, high quality NN scattering data are available.
Fit of all data gives reliable NN potential model
Argonne v18 : 4301 pp and pn elastic data were fit with c2/DOF ~ 1.09
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Short range part:Repulsive to saturate density
Stability of Nuclei
Max. Mass of Neutron Star
Supernova Explosion
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Long range part :Attractive to bind nuclei
Stability of Nuclei
Evolution of Stars
NucleosynthesisStructure of elements
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Klein-Gordon Equation
)(4)(
2
2
2
rdpf gmc
ct
Let m=0
)(4)( 2
2
rdpf ect
D’Alembert (Poisson) Equation : Stationary SolutionAs Jackson’s text book tells,
massless photon mediates EM force r
ef
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Klein-Gordon Equation
)(4)(
2
2
2
rdpf gmc
ct
Stational KG equation: Yukawa-potential
r
eg
r
f
mc
Let
Pion mediates nuclear force
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fm4.1MeV/140 12 p cm
One Pion Exchange
r
eg
r
f
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c
e
c
g
22
Dimension less Coupling Constants
~0.28 ~1/137 = 7.3x10-3
Electromagnetic ForceNuclear (Strong) Force
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Hit nucleus by size-zero particle : ElectronEM interaction is well known
Mott scattering (Rutherford scat. + spin) for finite size target:
dVfi
F
Fc
cEZ
d
d
)()exp()(
)(2
cos)(
2 22
2
2
xxqq
a
Form factor : Fourier transform of charge distribution
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J.B.Bellicard et al. PRL 19 (1967) 527.
MarkIII @ Stanford
F -1F-1
R.HofstadterNobel Prize in Physics 1961
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fm54.0~
1.1~
}/)exp{(1
)0()(
3/1
a
Ac
acrr
rr
r(0)*A/(Ze) ~ const = 0.17 / fm3
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Nucleon is Fermion : Subject to Pauli PrincipleFor simplicity : Assume Body Center Cubic Lattice
Nuclear Density is saturated :
r ~ 0.17/fm3
[(1/8 * 8 + 1)/0.17]1/3 ~ 2.3 fm
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Long range part :Attractive to bind nuclei
2.3 fm
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Nucleon behaves almost free in a nucleusNucleon is Fermion (subject to Pauli principle)
Treat nucleus as gas!
IsospinSpinei
rk1
L =L3
From B.C.
ii nL
kp2
nnn
n
dkkL
dkdk
dn 2
3
42
2 pp
# of States for Neutron
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3
20 3
1F
k
n
kdkdk
dnN
F
p
L =L3
Number of Neutrons : N
nnn
n
dkkL
dkdk
dn 2
3
42
2 pp
# of States for Neutron
3/1
23
NkF p
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3
20 3
1F
k
n
kdkdk
dnN
F
p
L =L3
Number of Neutrons : N
3/223/142
2
)9(
2
)(
N
MM
kE F
nF
p
Define Kinetic Energy of neutron
3/1
23
NkF p
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L =L3
3/223/142
2
)9(
2
)(
N
MM
kE F
nF
p
Kinetic Energy of proton
3/223/142
2
)9(
2
)(
Z
MM
kE F
pF
p
3/1
23
ZkF p
Define Kinetic Energy of neutron
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L =L3
Kinetic Energy of proton
3/223/142
2
)9(
2
)(
Z
MM
kE F
pF
p
3/1
23
ZkF p
Let N = Z = A/2, = A/0.17 [fm3]
MeV37~
MeV/260fm4.1~ 1
F
F
E
ck
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Proton
Neutron
Fermi Surface
Coulomb Repulsion
EF ~37MeV
B ~ 8MeV
V0 ~ 45 MeV for nucleon
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)(2
2
rp
UM
H
Fermi Gas : U = 0 Harmonic Oscillator : U = (½)Mw2r2
2
3nEn w
Shell structure : degeneracy g(n)
lnn r 2
( )( )212
1)12()(
2
nnlngnlnr
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Assumption! :Independent Particle ModelEffective interaction
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2 10 18 36 54 86
Can you guess the next number?
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Noble gases have closed shell for valence electrons.
2 10 18 36 54 86
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Ionization Energy of atoms
Z
Noble gases have closed shell for valence electrons.
2 10 18 36 54 86
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Magic Number
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Saxon- WoodsMeV50~
}/)exp{(1)(
0
0
V
aRr
VrV
sl )(rvVSO
Maria G. Mayer & J.H.D.Jensen1963 Nobel Prize in Physics : Shell Model
p-shellnuclei
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Spin Up
L = r x p
L ・S < 0 L ・S > 0
r
Classic Picture of LS force
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)12
1(
2
1)1()1(
2
1
)(
lljj
rvVSO
sl
sl
)12()(
2/1 )(
2/1 )1)((
21
21
21
lrvE
ljlrv
ljlrvVSO
J = l - ½Jack knife
J = l + ½Stretch
MeV20~)( 3/2 Arv
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With realistic interaction model (upto pf-shell)(195 parameters, 599 data were fit)E < 170keV
M.Homma et al.Phys.Rev. C 69 (2004) 034335.
s-shell
p-shell
sd-shell
pf-shell
Shell model calculation of heavy nuclei is difficult.
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Lots of NN scat. data
QCD
Various Data of Nuclei
NN Interaction Model
Nuclear StructureOrigin of Repulsive Core
Supernova
Nucleosysthesis
Quark Degree of Freedom
Quark Gluon PlasmaQuark matter
Nuclear Reaction
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Normal Nuclei (u, d)
Our World
NN interaction : Nuclear ForceShell Model
Hadron(Baryon + Meson)
Quark Gluon Plasma
YN ,YY interaction
NucleosynthesisSupernova
Big BangHigh T
Neutron Star
Hyperon/Quark StarOrigin of Mass
Quark Matter
RHIC, LHC
JLab
RIBF, GSIJPARC
Hypernuclear Physics
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N
Z L, S hypernuclei39 L1 S
stra
ng
en
ess
0
1
2
stableunstable
LL, X hypernuclei3 LL
Courtesy of M.Kaneta, H.Tamura
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14 June 2010 S N Nakamura @ Tohoku Univ.
Nuclear Force (NN) Baryon Force (YN,YY)
Nuclear Matter Baryon Matter(Neutron, Hyperon, Quark Stars)
Nuclear Structure Modified by impurity(Size, shape, symmetry…)
Baryon weak int.study is difficult
Hyperon weak decay and medium effect
n p
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(uds)
ct ~ 8cm
Scattering Exp. Difficult
Bound state can be formed
PDG (2010)
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L Strange Quark
Up Quark
Down Quark
Hyper NucleusProton
Neutron
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Extend Nuclear Force to Baryon Interaction
Use L as a probe to see deep inside of nucleus
Put L into nucleus as impurity
Test of the independent-particle modelquarks’ degree of freedom
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M.Yosoi et al.
s1/2
p3/2
p1/2
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L can probe deep inside of the nucleus
Convert a nucleon to L : free from nucleons’ Pauli Principle
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Long Range Part :
Nuclear Structure
Short Range Part : QCD pic.Repulsive CoreLS force
r (fm)
V(1 S
0) [
MeV
]
pp
p
,r,w
LN force : NO One Pion Exch (L : I0)
QCD
No One p ExchTwo p Exch.Heavier Meson Exch.
?
Density SaturationOrigin of Magic Number
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S N Nakamura for HKS/HES collaboration
Nucleus
n
L
K
p
A(K-,p-)LA reaction
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S N Nakamura for HKS/HES collaboration
Nucleus
n
L
K
p
A(p, K+)LA reaction
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S N Nakamura for HKS/HES collaboration
Nucleus
p
Le-
Z(e,e’K+)L(Z1) reaction
e-
K
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Probe to deep inside of the nuclei
L keeps its identity deep
inside of nucleus.
Spectroscopy of
the deeply bound L states
S N Nakamura for HKS/HES collaborationHotchi et al., PRC 64 (2001) 044302
Single particle nature of L
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YN scattering exp. is
very difficult
Oct. 25th 2007 S N Nakamura for E01-011 collaborationHotchi et al., PRC 64 (2001) 044302
Free YN int.
(meson/quark model)
Hyp. Nucl. Data
Effective YNFew body
G-matrix
Structure
Single particle nature of L
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S N Nakamura for E01-011 collaborationHotchi et al., PRC 64 (2001) 044302
Single particle nature of L
Various theoriesSkyrme HF (Yamamoto)DDRH (Lenske)Quark-meson coupling (Thomas,
Saito)etc….
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S N Nakamura for E01-011 collaboration
KEK-PS 2 MeV(FWHM)
Hypernuclear spectroscopy established
BNL 3 MeV(FWHM)
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1953 discovery of hypernucleus (emulsion with cosmic-ray, by Danysz and Pniewski)
Proton
pion
50m
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S N Nakamura @ Tohoku Univ.
1953 discovery of hypernucleus (emulsion with cosmic-ray, by Danysz and Pniewski)
1970s CERN, BNL Counter experiments with Kaon beam
Meson Beam @ CERN, BNL
A(K-,p-)LA reaction
Limitation by K intensity
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S N Nakamura @ Tohoku Univ.
1953 discovery of hypernucleus (emulsion with cosmic-ray, by Danysz and Pniewski)
1970s CERN, BNL Counter experiments with Kaon beam
1980s BNL-AGS, KEK-PS Counter experiments with K/p beam
Superconducting Kaon Spectrometer (SKS) @KEK-PS
Meson Beam @ BNL-AGS & KEK-PS
A(K-,p-)LA, A(p, K+)LA reaction
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S N Nakamura @ Tohoku Univ.
1953 discovery of hypernucleus (emulsion with cosmic-ray, by Danysz and Pniewski)
1970s CERN, BNL Counter experiments with Kaon beam
1980s BNL-AGS, KEK-PS Counter experiments with K/p beam
1998- g-spectroscopy with Hyperball
Hyperball2
Developed by H.Tamura’s Gr.
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S N Nakamura @ Tohoku Univ.
1953 discovery of hypernucleus (emulsion with cosmic-ray, by Danysz and Pniewski)
1970s CERN, BNL Counter experiments with Kaon beam
1980s BNL-AGS, KEK-PS Counter experiments with K/p beam
1998- g-spectroscopy with Hyperball
2000~
(e,e’K+) spectroscopy @ JLab
Z(e-,e’K+)L(Z1) reaction
HKS @Hall C
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Secondary Meson Beam (K-, p -) reaction @ BNL-AGS
(p,K) reaction @ KEK-PS
Energy resolution is limited by the meson beam quality
S N Nakamura for HKS/HES collaboration
About 2 MeV (FWHM) with SKS spectrometer at KEK
New method with high-quality primary beam
Hypernuclear production with (e,e’K+) reaction