Neutrino Nuclear Responses and Medium Energy Photons

Transcription

1 Neutrino Nuclear Responses and Medium Energy Photons Hiro Ejiri RCNP Osaka & CTU Praha Thanks Chary for invitation Saskatchewan 4-10

2 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

3 1. Neutrino studies in nuclei & neutrino nuclear responses Ejiri-weekend house at Shounan

4 Neutrinos, only weak charge, KEYs for particle astro and nuclear physics 1. Dirac /Majorana, ν anti ν ν e ν μ ν τ e μ τ 2. Mass hierarchy, NH m 1 <m 2 < m 3 IH m 3 <m 1 < m 2 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.

5 Majorana neutrinos and neutrino-less ββ decays. 0νββ A = B + β + β Lepton number ΔL=2 beyond SM. Particle physics Majorana ν, m ν CP T 0ν = G 0ν [M 0ν m ν ] 2 Nucl. physics. ν/weak responses τ σ correlation Cosmology DM Leptogenesis FEMTO(fm)-HC. to selectively enhance ν-exchange L N =10 48 cm -2 /s 1-ton L= cm -2 /s σ~10-83 cm 2 IH

6 D. Effective ν mass regions studied by ββ experiments KKDC 320meV QD 100~300 mev NEMOIII CUORITINO IH: mev CUORE MOOM EXO MAJORANA, NEMO θ 13 =0.2 NH: 2-5 mev Future R&D φ ι =α 2 α 1, φ ι = α 2 2δ Phase +/- ~ 2 IH/NH ~ 10 QD: Cosmological Σm i Single β ~ m ν = [Σ U i2 m i 2 ] 1/2 If IH and no 0νββ above 15 mev and ±ΔM 0ν 30%, we get Dirac ν ~ 200 mev

7 NaI 1 module 16 units PMT 1 unit X&Y fiber planes PMT PL plate PL plate ββ source film PMT

8 Detector Phase 1 Scintilation bolometer High E-resolution low BG, high sensitivity 1-Xal ZnMoO =125 cc ρ=4.3, 538g 95 % 100 Mo ratio= 41%, 222 g 8-Xal 100 Mo 1.8 k g 52 Xal 11.7kg CUORITINO 3 13x4=52Xal 5 3 =125cc Te0 2 41kg 130 Te=11kg Collaboration with Mlano-Rome group

9 Neutrino mass sensitivity CUORE 130 Te MOON PL 100 Mo MOON PS 100 Mo nd Phase 1 st Phase Neutrino mass sensitivity mev QD IH Exposure ton x year B C G

10 2. Nuclear weak/neutrino responses Ejiri s place at -Yokohama

11 Nuclear waek/ν responses for β &ββ, SN, the sun ν e e,ν e, ν ν e ν W W,Z W,Z n p n n n p τ, τσ τ, τσ τ, τσ β,ec, ββ SN EC, ν N interaction, ν-detection Solar ν, ν production, ν-detection Nuclear weak/ν responses Vector Fermi- Isospin τ Axial vector GT Spin Ispspin τσ

12 Nuclear responses for neutrinos 10 Relative strengths of 1 + and Solar ν / 2νββ SN ν e SN ν x 0νββ Sub.GeV N Medium Ε γ μ capture 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 , Ejiri P.R

13 H3 Nuclear responses for ββ ν Sensitivity of m ν = k [M 0ν ] -1 [N ββ /B] -1/4 in case of B>>1 1. M 0ν =<ττσσh(r)> is crucial for extracting m ν, IH/NH, phases, for designing exps. M 0ν 30% leads to N ββ detector 1/3 2. Sensitive to nuclear structures, τ σ corr., pp-correlation, effective g A, short-range. 3. Extremely small, 10-2 M SP, 10-4 M GR 4. 2νββ J π =1, 0νββ J π =1+,2-,3+, 6 for virtual ν q ~ 0.2 GeV Suhonen

14 スライド 13 H3 Ejiri, 2009/07/25

15 FSQP: Fermi Surface Quasi Particle Model GTR> 1 M 2ν (EXP) and M 2ν (FSQP) ββ k M 2νββ = Σ k M β km b k /Δ k =Σ k (g eff A) 2( m ij ) 2 V n U p V p U n /Δ k M 2ν (EXP), M 2ν (FSQP) Exp. values for M β km b k Mass number A 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 (g eff A) 2 ~ (0.25) 2 = 0.05 T 0ν ~ (g eff A) 4 = 0.002

16 Effective coupling constant: g A ~ (g A eff / g A ) ~ 0.24/0.01 A, nuclear medium σ τ correlations (στ GR interference). Effective coupling constant g eff A for 2νββ 10 g eff n A g eff /g β - and β Mass number A Mass number A g eff (β - ) ~ g eff (β + ) ~ 0.24, and [g eff (2νββ)] 2 = g eff (β - ) g eff (β * ) ~ 0.06 g pp cancellation is only for β+ (p-n) sides, but both are equal.

17 Nuclear Matrix elements from 0+ to 1 + and 2-10 J=1+ GT M(EXP) β - β J=2 [σ ry 1 ] M(EXP) 10-3 β β+ M(GT EXP) β - and β Mass number A Mass number M(1+) ~ 0.4 M(2-)~ g eff =M(1+)/M(SQP) ~0.25 g eff =(M(2-)/M(SQP) ~ 0.15 M 0ν =<ττσσh>, with h~ R/ r 1 -r 2, = R/[2<r> 3 ] M i M f,, Use exp. M i ~g eff M QP, M QP = <r> <τσy 1 > U V M 0ν ~ 0.01 for the lowest 2 - state, sum ~ 0.02, while QRPA ~ 0.8 with g eff ~ 1 (~0.02 with g eff ~ 0.15) GR?

18 Effective g A (g A ) 2 ~ 0.5 g A ~ 0.7 Nuclear medium effect g A ~ 1 (p,n) Frekers B(GT) and [g A ] 2 =B(GT)/3(N-Z) B(GT)/3(N-Z) B(GT) A Mass number

19 Nuclear τσ responses for ν in β &ββ Weak probe EM probe Nuclear probe τ, τσ τ, τσ ν e e e τ, τσ p, 3 He n,t W γ π,ρ n p N N n p β-decay EC, μ C MUSIC ν probe J-PARC SNS γ-capture, e scattering γ from Spring-8, HIGS CER 3 He,t t, 3 He d, 2 He N RCNP, MSU, KVI

20 3. Nuclear probes for ν nuclear responses

21 CER:Charge exchange reactions for τσ ν-weak responses RCNP ( 3 He,t) ( 7 Li, 7 Be), MSU (t, 3 He), KVI (d, 2 He) Munster (Frekers ) MSU (Zegers) RCNP (Akimune, Ejiri,Fujiwara) E/A~0.2 GeV, LargeV(τσ), small V 0 I. Start ~ ββ PL solar-ν 98 PL II 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

22 Energy Resolution ΔE/E ~ 0.005% RCNP Cyclotron Facility Ring Cyclotron K=400 MeV ΔE/E ~ 0.01% Injector Cyclotron K=140 MeV Upgraded recently

23 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

24 Ga Solar ν responses B(GT)= Ga (pp-ν) 71 Ge Ge log ft = 4.3 (B(GT)=0.09) Q =229.4 kev EC Akimune, Ejiri, Frekers, Zegers et al Preliminary data 10 GT Full I i -I f B(GT) σ(0) L 3/2-1/ /2-5/ Weak p3/2 f5/2 is mainly due to L=2 and tensor

25 Neutrino response Project ββ and astro-neutrinos with 2 -,weak 1 +, DCER, β 3 He,t RCNP ΔE/E = 0.03/450 β + d, 2 He 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)

26 4. Photon Probes for ν nuclear responses

27 Photon γ 1. Neutral current responses Isospin rotation for charged current responses via IAS Isobaric Analogue State β 3. Vector/E1 & axial vector/m1 γ P γ (L) angle distribution T - Spring-8 T - B A B β γ γ Z - γ W N P γ A A A T - isospin rotation

28 New SUBARU ΗΙγS

29 γ decays through IAS for charged weak currents <f g M β i> = g/e (2T) 1/2 <f em γ IAS> r, σ, r x σ by E1 and M1 γ Excited states i > in B by IAS of i > = T- i >. Τ =ΙΑS Τ,Tz=5,4 Excited states of f> by γ decays to f >. Β Τ,Τz=5,5 ββ β γ Α Τ,Τz=4,4 H. Ejiri PRL 21 68, H. Ejiri PR 38 78

30 p + Α = ΙΑS + γ and GR + γ Phases from interference with giant resonances. H. Ejiri PRL 21 68, H. Ejiri PR 38 78

31 IAS γ and analogue β matrix elenments HIGS I γ ~ 10 8 /0.2 MeV, T ~ 30 mg Γ t ~ 0.2 MeV B(EM1) σ(em 1) mb Y/se E1 0.5/(2T) M1 0.3/(2T)

32 5. Lepton probes for ν nuclear responses

33 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 Y 1 GR μ capture No of n and γ & their E strength distribution. Calibrate by p/a captures.

34 Low energy Neutrinos H. Ejiri NIM. 503 (2003) p + Hg n π + π + μ + +ν μ μ + e + + ν e + anti-ν μ Avignone ORNL E p Gev N p /sec N n /sec SNS J-PARC GeV 50 GeV J-PARC

35 5. Concluding remarks Ejiri s place at Yokohama

36 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 ( 3 He, 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.

37 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 3 He, 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.

38 Thank you for your attention Ejiri7s weekend house at Shounan