京大講義パート2�（6月20日）�Nenbutsu-dera in KyotoHisakazu Minakata	U. Sao Paulo	Overseeing Copacabana beachfrom Pão de Açúcar

All the angles are measured !
lepton CP phase δ left	SK-atm+MINOS+T2KJune 20, 2014	T2K-MINOS-DC-DB-RENONeutrino Kogi@Kyodai	να=Uαi νi�solar+KamLANDJune 20, 2014	

Neutrino Kogi@Kyodai	Solar ν (in a nutshell)�• Sun shines because of net reaction
ppppà4He + 2e+ + 2νe + 25MeV	• By knowing the solar constant = SC =0.136 W/cm2, the solar neutrino flux F at the earth isgiven by:	• F = 2x (0.136/25) (J s/cm2 MeV) 	• 1 MeV = 1.60 x 10-13 J	• F = 6.8 x 1010 (1/s cm2)�June 20, 2014	Neutrino Kogi@Kyodai	Chain of nuclear reaction in the Sun is a bit more complex�June 20, 2014	Neutrino Kogi@Kyodai	Chain of nuclear reaction in the Sun�June 20, 2014	Neutrino Kogi@Kyodai	Standardsolarmodel: one
can modelinterior ofthe Sun�June 20, 2014Neutrino Kogi@KyodaiCalculated result of solar neutrino flux�June 20, 2014	Neutrino Kogi@Kyodai	Chain of nuclear reaction in the Sun is a bit more complex�June 20, 2014	Neutrino Kogi@Kyodai	LENA@Gran Sasso Lab.

June 20, 2014	Neutrino Kogi@Kyodai	June 20, 2014	Neutrino Kogi@Kyodai	June 20, 2014	Neutrino Kogi@Kyodai	June 20, 2014	Neutrino Kogi@Kyodai	Chain of nuclear reaction in the Sun: Again�Main engine of the Sun�June 20, 2014	Neutrino Kogi@Kyodai	37Cl and 71Ga experiments: Radio-chemicalexperiments	• Homestake (Ray Davis): νe+37Cl -> e-+37Ar(Pioneer!)	• Ga experiment: νe+71Ga -> e-+37Ge 	• Sensitive only to νe	• Low energy threshold	June 20, 2014	Neutrino Kogi@Kyodai	Results of 37Cl experiment:production rate of 37Ar�1 SNU = 10−36events / (No.
of target atomsec)�~1/3 of SSMexpectation:solar nuproblemstarted!
June 20, 2014	Neutrino Kogi@Kyodai	SAGE(60 t),	GALLEX/GNO (30 t)�~60% ofSSMprediction�June 20, 2014	Neutrino Kogi@Kyodai	1st experimentwhich proved thatneutrinos comesfrom the Sun �

June 20, 2014	Kamiokande II�Neutrino Kogi@Kyodai	June 20, 2014	Neutrino Kogi@Kyodai	Precision SK measurement Now� Koshio Nu2014�June 20, 2014	Neutrino Kogi@Kyodai	2039m underground�June 20, 2014	Neutrino Kogi@Kyodai	June 20, 2014	Neutrino Kogi@Kyodai	June 20, 2014	Neutrino Kogi@Kyodai	June 20, 2014	

Neutrino Kogi@Kyodai	Solar ν spectrum consistent with MSW�Pee = 1-(1/2)
c134 sin22θ12�Pee =sin2θ12�June 20, 2014�

Neutrino Kogi@Kyodai�Reactoris a richsource ofneutrinos�June 20, 2014	Neutrino Kogi@Kyodai	June 20, 2014	

Used by Reines-Cowan toobserve νe-bar for the first time�Neutrino Kogi@Kyodai	2 different regimes of reactorneutrino oscillationνe disappearanceprobability�June 20, 2014	Neutrino Kogi@Kyodai	With which baseline L neutrinososcillate?�June 20, 2014	

Neutrino Kogi@Kyodai	KamLAND@Kamiokamine�June 20, 2014	Neutrino Kogi@Kyodai	KamLAND: Modulation of energyspectrum�June 20, 2014	Neutrino Kogi@Kyodai	The cleanest evidence for neutrinoOSCILLATION�June 20, 2014	Neutrino Kogi@Kyodai	�SNO(+SK)
andKamLANDsolved thesolarneutrinoproblem   June 20, 2014	

Neutrino Kogi@Kyodai	20151052m
1m(b)KamLAND+Solar KamLAND95% C.L.

95% C.L.

99% C.L.

99% C.L.

99.73% C.L.

99.73% C.L.

best-fit

best-fit

4m

June 20, 2014	

3m

3m

2.2
21.81.61.41.2
10.8
0.60.40.24m

2m1m26m21(10-4eV 2)6r 2Determination of θ12, Δm221Solar95% C.L.
99% C.L.
99.73% C.L.
best-fite13 constrained0.1 0.2 0.3 0.4 0.50.6 Kogi@Kyodai	0.7 0.8 0.9 1 5 10 15 20Neutrinotan2 e6 r2θ12 and θ13�• sin2θ12 = 0.304 +/- 0.013	• Error of sin2θ12 = 4.3%	• Error of Δm221 = 2.4%		KamLAND+solar Mar.2013Daya Bay Nu2014��• Error of sin2θ13 (Daya Bay) = 6.1%	• Error of Δm231 (Daya Bay) ~= 4% !!	

2 (MINOS) ~= 4%	

• JuneErrorofΔm31
20, 2014�Neutrino Kogi@Kyodai�What’s new
in 12 sector?�June 20, 2014	Neutrino Kogi@Kyodai	Day-night variation seen! (SK)�Koshio Nu2014�June 20, 2014�Neutrino Kogi@Kyodai�Spectrum upturn seen though still at 1σ level(SK) �June 20, 2014�Neutrino Kogi@Kyodai�Cosmic rays are arriving at the Earth�June 20, 2014	Neutrino Kogi@Kyodai	Cosmic ray energy spectrum�1 particle / m2 sec�1 particle / m2 year�1 particle / km2 year�June 20, 2014	Neutrino Kogi@Kyodai	Zenith angle dependence of atmosphericneutrinos �What is zenith angle?�

June 20, 2014	Upward
going�Neutrino Kogi@Kyodai	Downward going�June 20, 2014	Neutrino Kogi@Kyodai	R.Wendell Nu2014�June 20, 2014	Neutrino Kogi@Kyodai	June 20, 2014	Neutrino Kogi@Kyodai	R.Wendell Nu2014�June 20, 2014	Neutrino Kogi@Kyodai	In anutshell  June 20, 2014Neutrino Kogi@KyodaiFocus in on µ-like events	• Pay attention to the high energy(p > 400 MeV) events	

• Downward-going events agreeswith Monte Carlo	• But, a large discrepancy existsin upward-going events =neutrinos from the other side ofthe earth (from Brazil!) 	• Neutrino oscillation takesplace with oscillation lengthof ~1000 km	June 20, 2014	Neutrino Kogi@Kyodai	With which baseline L neutrinos oscillate?�June 20, 2014	Neutrino Kogi@Kyodai	Acceleratorneutrinos:Tokai-toKamioka(T2K)�June 20, 2014	Neutrino Kogi@Kyodai	June 20, 2014	Neutrino Kogi@Kyodai	June 20, 2014	Neutrino Kogi@Kyodai	June 20, 2014	Neutrino Kogi@Kyodai	June 20, 2014	Neutrino Kogi@Kyodai	What’s newin 23 sector?  

June 20, 2014	Neutrino Kogi@Kyodai	θ23 2nd octant, δ ~ 3π/2 preferred ?�R.Wendell Nu2014�June 20, 2014�Neutrino Kogi@Kyodai�Accelerator θ23 sensitivity better thanSK atm’s�Mild preference ofnormal hierarchy�June 20, 2014	Neutrino Kogi@Kyodai	How tomeasure θ13 ?

June 20, 2014	Neutrino Kogi@Kyodai	To measure θ13 one needs νe	• P(νe -> νe) is the interference between 	e->1 -------> 1->e and e->2 -------> 2->ee->3 -------> 3->e	Obviously involve|Ue3|2 = s213		• P(νµ -> νe) is the interference between 	µ->1 -------> 1->e and µ->2 -------> 2->e 	µ->3 -------> 3->e	 Involve |Ue3|= s13but in fact s213�Reactor and accelerator are equally good probe for θ13June 20, 2014	Neutrino Kogi@Kyodai	Reactor measurement of θ13�

Double Chooz �June 20, 2014	Neutrino Kogi@Kyodai	2 different regimes of reactorneutrino oscillationneed to measuresmall νe deficit !�Independent of δ, θ23,
matter effect, θ12, solar
Δm2 à puremeasurement of θ13June 20, 2014	Neutrino Kogi@Kyodai	Near-far “identical” 2 detectors�June 20, 2014	Neutrino Kogi@Kyodai	June 20, 2014	Neutrino Kogi@Kyodai	June 20, 2014	Neutrino Kogi@Kyodai	13 sector: beautiful result from Daya Bay�Chao Zhang Nu2014�June 20, 2014�Neutrino Kogi@Kyodai�Acceleratormeasurementof θ13  June 20, 2014	Neutrino Kogi@Kyodai	June 20, 2014	Neutrino Kogi@Kyodai	θ12 and θ13�• sin2θ12 = 0.304 +/- 0.013	• Error of sin2θ12 = 4.3%	• Error of Δm221 = 2.4%		KamLAND+solar Mar.2013Daya Bay Nu2014��• Error of sin2θ13 (Daya Bay) = 6.1%	• Error of Δm231 (Daya Bay) ~= 4% !!	

2 (MINOS/T2K) ~= 4%	

• JuneErrorofΔm31
20, 2014�Neutrino Kogi@Kyodai�Then what’snext?
ν Masspattern:“masshierarchy”and CP	June 20, 2014	Neutrino Kogi@Kyodai	Mass hierarchy resolution and CP:understanding the principle�
Use matter effect to determinethe ν mass hierarchy 	Use P – P-bar asymmetry +spectral modulation tomeasure CP phase δ 	June 20, 2014�Neutrino Kogi@Kyodai�Sensitivity to masshierarchy by LBL: limitedfor the time beingNOVA +T2K	SK-atm	

Lucky regions	June 20, 2014�Neutrino Kogi@Kyodai�Use of atmospheric ν for mass hierarchy:(PINGU, Hyper-K, LBNE)�PINGU	σE=2 GeVσθ=11.25o�AkhmedovRazzaque-SmirnovJune 20, 2014	June 12�e-like larger fornormal hierarchy �MSWNeutrino Kogi@Kyodai	resonance�How tomeasure δ?   
Not easy because ofdouble suppression:J_r and Δm221/Δm231�June 20, 2014	Neutrino Kogi@Kyodai	How oscillation probability inmatter depend on θ13–θ23– δ ? �
8L = 810 km E = 2.0 GeVδ=0δ = π/2δ=πδ = 3π/222

sin 2θ23 = 0.5mat2terΔm 31 < 05~vacuumctsin

δ234in 2θ2~

sin 22θ13 s

Δm 31 > 0sδ

32effe~P(νµνe) [%]6co7sin 2θ13 = 0.11
M-N: JHEP10(2001)0010

0123P(νµ45νe) [%]67Bi-P plot: dependence onθ13,Juneθ2320,, 2014�and δ displayedpictorially	8Neutrino Kogi@Kyodai	Hyper-Kamiokande: CP sensitivity �Normal hierarchy�June 20, 2014	Neutrino Kogi@Kyodai	Summary�• First hint for nonzero ν mass came fromsolar ν, but first evidence was from SK
atmospheric ν (23 oscillation)• KamLAND and solar ν experiments jointlyfound another channel oscillation/flavorconversion (12 oscillation)• All the mixing angles are now measured (stillconsistent with 3 ν scheme)• ν mass hierarchy and CP δ left• I failed to cover Majorana vs Dirac,Majorana phase, absolute neutrino massscale etc.
June 20, 2014�Neutrino Kogi@Kyodai�