Neutrino Nuclear Responses and
Medium Energy Photons
Hiro Ejiri
RCNP Osaka & CTU Praha
Thanks Chary for invitation
Saskatchewan 4-10
1. Neutrino studies in nuclei &
neutrino nuclear responses
2. Neutrino/weak nuclear responses
3. Nuclear probes for ν nuclear responses
4. Photon probes for ν nuclear responses
5. Lepton probes for ν nuclear responses
6. Concluding remarks
1. Neutrino studies in nuclei &
neutrino nuclear responses
Ejiri-weekend house at Shounan
Neutrinos, only weak charge, KEYs for
particle astro and nuclear physics
1. Dirac /Majorana , ν ≠anti ν
2. Mass hierarchy, NH m1<m2 < m3
νe νμ ντ
e μ τ
IH m3<m1 < m2
3. Flavor mixing and mass differences, but absolute mass ?
4. Lepton sector CP phases ?
5. Leptogenesis for B asymmetry?
6. Astro (solar, supernova) ν production, synthesis, & detection
7. Nuclear weak responses and spin isospin correlation
These fundamental questions are studied in nuclei ,
where nuclear ν/weak responses are crutial.
Majorana neutrinos and
neutrino-less ββ decays
0νββ
A=B+β+β
Lepton number ΔL=2 beyond SM.
.
Particle physics
Majorana ν, mν CP
T0ν = G0ν [M0ν mν]2
Nucl. physics.
ν/weak responses
τ σ correlation
Cosmology
DM
Leptogenesis
FEMTO(fm)-HC.
to selectively enhance
ν-exchange
LN= 1048cm-2 /s
1-ton L= 6 1075cm-2 /s
σ~10-83cm2 IH
D. Effective ν mass regions studied by ββ experiments
QD 100~300 meV
KKDC 320meV
NEMOIII CUORITINO
IH: 20-50 meV
CUORE MOOM EXO
MAJORANA, NEMO
NH: 2 - 5 meV
θ13=0.2
φι=α2−α1, φι = α2−2δ
Phase +/- ~ 2 IH/NH ~ 10
Future R&D
QD: Cosmological
Σmi
Single β ~ mν = [Σ Ui2 mi 2]1/2 ~ 200 meV
If IH and no 0νββ above 15 meV and ±ΔM0ν 30%, we get Dirac ν
1 module
16 units
NaI
PMT
1 unit
X&Y fiber planes
PL plate
PMT
PL plate
ββ source film
PMT
Detector Phase 1
Scintilation bolometer
High E-resolution low BG,
high sensitivity
1-Xal
ZnMoO4 53=125 cc ρ=4.3 , 538g
222 g
95 % 100Mo ratio= 41%,
8-Xal 100Mo
52 Xal
1.8 k g
11.7kg
３
CUORITINO
13ｘ４＝52Xal ５３＝１２５ｃｃ
Te02 41ｋｇ １３０Te＝11ｋｇ
Collaboration with Mlano-Rome group
Neutrino mass sensitivity
CUORE 130Te MOON PL 100Mo MOON PS 100Mo
2nd Phase
2012
1st Phase
Neutrino mass sensitivity meV
1000
B
C
G
100
QD
IH
10
0.01
0.1
Ex po su re
1
to n x ye a r
10
2. Nuclear weak/neutrino responses
Ejiri’s place at -Yokohama
Nuclear waek/ν responses for β &ββ, SN, the sun
ν
e
W
n
n
eν
ν
W,Z
p
τ, τσ
e, ν
e,ν
W,Z
n
n
τ, τσ
p
τ, τσ
β,EC, ββ
SN EC,
ν –N interaction,
ν- detection
Nuclear weak/ν responses
Vector Fermi- Isospin τ
Axial vector GT Spin Ispspin τσ
Solar ν,
ν –production,
ν- detection
Nuclear responses for neutrinos
Relative strengths of 1+ and 2-
10
Solar ν / 2νββ SN νe SN νx 0νββ
1
0.1
0.01
Sub.GeV N
Medium Ε γ
μ capture
0.001
0.0001
1
10
100
Neutrino momentum MeV/c
Sub.GeV σ τ responses of GT(L=0) and SD(L=1) are modified
by σ τ correlations. giant resonances and nuclear medium effects
Ejiri Fujita P.R. 38 1978 85, Ejiri P.R. 338 2000 265
H3
Nuclear responses for ββ−ν
Sensitivity of mν = k [M0ν]-1 [Nββ/B]-1/4 in case of B>>1
M0ν=<ττσσh(r)> is crucial for extracting mν , IH/NH, phases,
for designing exps. M0ν 30% leads to Nββ detector 1/3
2. Sensitive to nuclear structures, τ σ corr., pp-correlation,
effective gA , short-range.
3. Extremely small, 10-2 MSP, 10-4 MGR
4. 2νββ Jπ=1, 0νββ Jπ=1+,2-,3+, 6 for virtual ν q ~ 0.2 GeV
1.
Suhonen
スライド 13
H3
Ejiri, 2009/07/25
FSQP: Fermi Surface Quasi Particle Model
M2ν (EXP) and M2ν(FSQP)
|GTR>
M2ν(EXP), M2ν(FSQP)
1
|k
ββ
b /Δ
= Σk
M
k
k
k
=Σk (geffA)2 (mij)2VnUpVpUn/Δk
M2νββ
Mβ
Exp. values for
Mβ
b
kM k
0.1
0.01
0.001
70
80
H. Ejiri, Phys. Report 338 (2000) 265.
H. Ejiri et al. J. Phys. Soc. Japan Lett. 65 (1996) 7.
Η. Ejiri J. Phys. Soc. Japan, 78 (2009) No 7.
H. Ejiri Prog. Nuclear Particle Physics, 2009
90
100
110
120
130
Mass number A
(geffA)2 ~ (0.25)2 = 0.05
T0ν ~ (geffA)４ = 0.002
140
Effective coupling constant: gA~ (gAeff / gA) ~ 0.24/0.01 A,
nuclear medium σ τ correlations (στ GR interference).
10
geff/g β- and β+
Effective coupling constant geff A for 2νββ
geffn
A
1
0.1
1
0.1
0.01
0.01
70
80
90
100
110
Mass number A
120
130
140
70
80
90
100
110
120
130
Mass number A
geff (β-) ~ geff (β+) ~ 0.24 , and [geff (2νββ)]2= geff (β-) geff (β*) ~ 0.06
gpp cancellation is only for β+ (p-n) sides, but both are equal.
140
Nuclear Matrix elements from 0+ to 1+ and 2J=1+ GT M(EXP) β -
J=2 − [σ rY 1 ] M(EXP) 10-3 β − β +
β+
M(GT EXP) β- and β+
10
100
10
1
1
0.1
0.1
0.01
70
80
90
100
110
120
130
Mass number
140
0.01
60
80
100
120
140
A Mass number
M(1+) ~ 0.4
geff =M(1+)/M(SQP) ~0.25
M(2-)~0.7 10-3
geff =(M(2-)/M(SQP) ~ 0.15
M0ν=<ττσσh>, with h~ R/|r1-r2|,
= R/[2<r>3] Mi Mf,, Use exp. Mi ~geff MQP, MQP = <r> <τσY1> U V
M0ν ~ 0.01 for the lowest 2-state, sum ~ 0.02, while
QRPA ~ 0.8 with geff ~ 1 (~0.02 with geff ~ 0.15) GR ?
Effective gA
(gA)2 ~ 0.5
gA ~ 0.7
Nuclear medium effect
gA ~ 1 (p,n)
B( GT ) a n d [g A]2= B ( G T) /3 (N -Z )
B(GT)
Frekers
B(GT)/3(N-Z)
10
1
0.5
0.1
50
60
70
80
90
A Mass number
100
Nuclear τσ responses for ν in β &ββ
Weak probe
ν
τ, τσ
W
n
e
p
β-decay EC,
μ C MUSIC
ν probe
J-PARC SNS
EM probe
e
τ, τσ
Nuclear probe
e
p,3He τ, τσ
π,ρ
γ
N
n,t
N
γ-capture,
e scattering
γ from
Spring-8, HIGS
p
n
CER 3He,t
t,3He d,2He
N RCNP,
MSU, KVI
3. Nuclear probes for
ν nuclear responses
CER:Charge exchange reactions for τσ ν-weak responses
RCNP (3He,t) (7Li, 7Be), MSU (t,3He), KVI (d,2He)
Munster (Frekers ) MSU (Zegers) RCNP (Akimune, Ejiri,Fujiwara)
E/A~0.2 GeV, LargeV(τσ), small V0
I. Start ~ ββ 1995 ’97 PL solar-ν ’98 PL
II. 2007 - ΔE ~10-4, Freckers Ejiri et al, Zegers et al.
V(weak) ≠V(strong), Non-central V, distortion, multi-step, etc.
CER q-dependence and EC/β rates are used to get weak responses
RCNP Cyclotron Facility
Energy Resolution
ΔE/E ~ 0.005%
Ring Cyclotron
K=400 MeV
ΔE/E ~ 0.01%
Upgraded recently
Injector Cyclotron
K=140 MeV
Frekers
MeV
One or several low-lying 1+ states of [g7/2 g9/2] etc
One or several low-lying 2- states of [h11/2 g7/2] etc.
These contribute to 2νββ and 0νββ processes
Solar ν responses
32
71Ga
(pp-ν)71Ge
Akimune, Ejiri,
Frekers, Zegers et al
499.9
52
Preliminary data 10
174.9
1B(GT)=0.005 2
32
71
Ga
31
GT
Full
71
Ge
31
log ft = 4.3
(B(GT)=0.09)
Q
=229.4 keV
EC
Ii-If
3/2 - 1/2
3/2 - 5/2
B(GT)
0.1
0.002
σ(0)
1
2
L
0
2
Weak p3/2 – f5/2 is mainly
due to L=2 and tensor
Neutrino response Project
ββ and astro-neutrinos with 2- ,weak 1+, DCER,
β− 3He,t RCNP ΔE/E = 0.03/450
β+ d,2He KVI BBS (Δφ=60 mr, Δθ=140 mr, Δp=±15% ΔE/E = 0.1/185)
RCNP LAS (Δφ=240mr, Δθ=125 mr, Δp=±15% ΔE/E = x /200)
4. Photon Probes for ν nuclear responses
Photon γ
1. Neutral current responses
1. 2. Isospin rotation for
charged current responses via
IAS Isobaric Analogue State
β
Spring-8
3. Vector/E1 & axial vector/M1 γ
Pγ(L) angle distribution
T -B
γ
A
Z-γ
A
T-
B
W
A
N
A
T- isospin rotation
γ
β
P
γ
New
SUBARU
ΗΙγS
γ decays through IAS for charged weak currents
<f |g Mβ| i> = g/e (2T)1/2 <f | emγ | IAS>
r, σ, r x σ by E1 and M1 γ
Τ,Tz=5,4
Excited states |i’> in B by
IAS of |i’> = T-|i’>.
Excited states of |f> by
γ decays to |f’>.
Τ− =ΙΑS
γ
Β Τ,Τz=5,5
ββ
β
Α Τ,Τz=4,4
H. Ejiri PRL 21 ’68, H. Ejiri PR 38 ‘78
p + Α = ΙΑS + γ and GR + γ
Phases from interference with giant resonances.
H. Ejiri PRL 21 ’68, H. Ejiri PR 38 ‘78
IAS γ and analogue β matrix elenments
HIGS Iγ ~ 10８/0.2 MeV, T ~ 30 mｇ Γt ~ 0.2 MeV
B(EM１）
E1 0.5/(2T)
M1 0.3/(2T)
σ(EM 1) mb
2.0
0.15
Y/se
50
4
5. Lepton probes for ν nuclear responses
Weak strength distribution by μ-capture and deca
H. Ejiri, et al., Proc. e-γ Sendai 1972,
NP. 305 (1978) 167
xn,γ
τ+σ Y1
GR
μ capture
No of n and γ & their E
strength distribution.
Calibrate by p/a captures.
Low energy Neutrinos
H. Ejiri NIM. 503 (2003) 276 – 278.
p + Hg Æ n π+
π+ Æ μ+ +νμ
μ+ Æe+ + νe + anti-νμ
Avignone ORNL
3 GeV
Ep Gev Np /sec Nn/sec
SNS
1
6 1015
1 1015
J－PARC 3
1.2 1015 5 1014
50 GeV
J-PARC
5. Concluding remarks
Ejiri’s place at Yokohama
Concluding Remark
１．Neutrinos, the key particles for new particle and astro
nuclear physis, Nuclear ν/weak responses with q <1/fm are
crutial for ν-studies in ββ and astro (solar/SN) ν studies.
2. Neutrino/weak nuclear responses are very sensitive to
nuclear σ τ correlations and nuclear medium effects.
3. Neutrino/weak responses are studied by nuclear probes
(CER and inelastic scatterings), EM photon probes(γ-IAS,
γ capture), and lepton probes(β, ββ, EC, μ, ν-probes).
2νββ responses are reproduced by using β, EC, CER data
4. RCNP (3He, d. p) and MSU t probes, the NewSUBARU
/HIGS and CLS γ probes, RCNP, SIN μ and
J- PARC ν probes are used for studying ν responses.
NEWIN
Neutrinos & Electro-Weak Interactions in Nuclei
1.Astronuclear ν-weak responses and ν nuclear physics
2. International open network of independent groups
3. Objective Coordinated and collaboration efforts for
*ν /weak responses with q~1/fm and J=2-, 1+,
and so on for 0νββ and astro (SN, sun) ν’s.
* Neutrino-less ββ-decays in nuclei for QD and IH
4. Exp. probes
RCNP 3He, d, and p probes, MSU t probes
NewSUBARU/HIGGS/ CLS γ probes
μ/MUSIC and J-PARC/SIN ν R&D
5. Theory probes QRPA, shell model, others.
Thank you for youｒ attention
Ejiri7s weekend house at Shounan