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Based on J. Hisano, T. Kuwahara, N. Nagata, Phys. Lett. B723 (2013) 324, J. Hisano, D. Kobayashi, T. Kuwahara, N. Nagata, JHEP 1307 (2013) 038, N. Nagata, S. Shirai, JHEP 1403 (2014) 049.

1. Introduc+on 2. High- scale Supersymmetry 3. SUSY GUT in high- scale SUSY 4. Proton Decay in high- scale SUSY 5. Conclusions and discussion

1. Introduc,on

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60 N. Sakai (1981) S. Dimopoulos and H. Georgi (1981) 50 40 α -1 30 U(1) SU(2) 20 10 SU(3) 0 2 4 6 8 10 12 14 16 18 Log 10 (Q/GeV) S. P. Mar+n, arxiv: 9709356

SUSY SM TeV EW

SUSY SM [GeV] m 1/2 700 600 MSUGRA/CMSSM: tanβ = 10, A = 0, µ>0 0 ATLAS -1 L dt = 4.7 fb, Combined s=7 TeV SUSY Observed limit (±1 σ ) theory Expected limit (±1 σ exp ) TeV τ 500 LSP 400 ~ q (1000) ~ q (1400) q ~ (1800) -1 PLB 710 (2012) 67-85, 1.04 fb LEP Chargino ~ No EWSB g (1200) ~ g (1000) EW 300 200 ~ q (600) ~ g (600) ~ g (800) 500 1000 1500 2000 2500 3000 3500 4000 m 0 [GeV]

SUSY SM Events / 2 GeV 3000 2500 2000 1500 TeV 1000 EW g 3500 ATLAS 500 200-1 s=7 TeV, Ldt=4.8fb -1 s=8 TeV, Ldt=5.9fb (a) Data Sig+Bkg Fit (m =126.5 GeV) H Bkg (4th order polynomial) τ 500 LSP 400 H 300 200 ~ g (600) [GeV] m 1/2 700 600 MSUGRA/CMSSM: tanβ = 10, A = 0, µ>0 0 ~ q (600) ~ q (1000) ~ q (1400) q ~ (1800) ATLAS -1 L dt = 4.7 fb, Combined s=7 TeV SUSY Observed limit (±1 σ ) theory Expected limit (±1 σ exp ) -1 PLB 710 (2012) 67-85, 1.04 fb LEP Chargino ~ No EWSB g (1200) ~ g (1000) ~ g (800) 500 1000 1500 2000 2500 3000 3500 4000 m 0 [GeV]

Ø ( stop ) Ø ( CP ) Ø Ø w/ ( )

N. Sakai, T. Yanagida (1982) S. Weinberg (1982) H. Murayama and A. Pierce (2002) Super- Kamiokande

2. High- scale Supersymmetry

(M Pl : the reduced Planck scale)

Scalar Par cles Gravi no Higgsinos Gauginos ( ) Gluino Bino Wino

質量スペクトル Scalar Par!cles Gravi!no Higgsinos MS = 10(2-4) TeV Gauginos (ループ因子の分軽くなる) ヒッグス質量を説明 mh>127gev Gluino tanb 10 Bino 135GeV Wino 130GeV tanβは小さい 125GeV 120GeV mh<115.5gev 1 10 102 MSUSY êtev 103 104 M. Ibe, S. Matsumoto, T. Yanagida (2012)

Scalar Par cles Gravi no Higgsinos M S = 10 (2-4) TeV Gauginos ( ) Gluino Bino Wino O(1) TeV pure gravity media.on, M. Ibe, T. Moroi, T. T. Yanagida (2007) simply unnatural supersymmetry, N. Arkani- Hamed, et.al. (2012) spread supersymmetry, L. J. Hall and Y. Nomura (2012) mini- split, A. Arvanitaki, et.al. (2012)

3. SUSY GUT in high- scale SUSY

S. Dimopoulos and H. Georgi (1981) N. Sakai (1981) (M HC : )

SU(5) SU(3) C SU(2) L U(1) Y

J. Hisano, H. Murayama, T. Yanagida (1992).

(1- loop in DR scheme)

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M Hc 10 18 10 17 10 16 10 15 M 3 /M 2 = 3 M 3 /M 2 = 9 M 3 /M 2 = 30 10 2 10 3 μ H = M S M 2 = 3TeV tanβ = 3 M S (TeV) J. Hisano, T. Kuwahara, N. Nagata, Phys. Leb. B723 (2013) 324.

μ H = M S M S = 10 3 TeV tanβ = 3 M GUT M 2 = 300GeV 10 16 M 2 = 3TeV 10 1 M 3 (TeV) M GUT J. Hisano, T. Kuwahara, N. Nagata, Phys. Leb. B723 (2013) 324.

50 U(1) 28 High- scale SUSY α 1 40 30 20 10 SU(2) SU(3) 10 6 10 8 10 10 10 12 10 14 10 16 Scale (GeV) α 1 Zoom 27 26 25 10 16 Scale (GeV) Low- scale SUSY

4. Proton decay in high- scale SUSY

2 6 + 2 9 9 2 = 6 + 4 + 2 CKM

Q i Q k U i U k H C H C H C H C LLLL Q i L l E j D l RRRR LLLL RRRR

LLLL RRRR

At SUSY scale g, W, B, H u,d

Minimal Flavor Viola+on q L q L ll ( q L ) q L (l L ) d R (s R ) t R τ R u R W H u Hd q L (a) LLLL l L (q L ) s L (d L ) (b) RRRR (ν τ ) L T. Goto and T. Nihei (1999) V. Lucas and S. Raby (1997) μ H >> M 2

2 J. Raaf, NNN 2013 Super- Kamiokande amiokande ure water m.w.e.) in Kamioka ch Inner PMTs Outer D) PMTs 00% 1996年開始 22500 ton の水を用いたチェレンコフ検出器 Atmospheric%ν% ~1% GeV% cos c = 1/n TeV% チェレンコフ光から電子とミューオンを区別できる

Hyper- Kamiokande Lifetime limit 90 CL (years) 10 36 Hyper-Kamiokande 10 35 Super-Kamiokande 10 34 10 33 2010 2015 2020 2025 Year 2030 2035 2040

p K+ν + + in Water!K Cherenkov + in Water Chere!K in inwater Water!K Cherenkov Cherenkov 1, 2013,# /.#0.-# J. Raaf, NNN 2013 November 11, 2013 23 J. Raaf, NNN 2013 *#+(,# *#+(,# -.//.#0.-# -.//.#0.-# $%&# *#+(,# Improvements in Improvements in -.//.#0.-# $%&#$%&# p νk+ p νk+ $'()# 64 % $'()#$'()# $%&# 21 % $'()# momentum reconstruction Better momentum reconstruction gging efficiency!"#$ %&'($)*+,-./,0$!"&$$!"1$ %2,3$,4,)5-*26)70$!"8$ + 4はチェレンコフ光を出す敷居を超えないので "10.-#.23## #4 5# 5#γ-tagging efficiency!"#$ %&'($)*+,-./,0$!"&$$!"1$ %2,3$,4,)5-*26)70$!"8$ K & es atmospheric ν BG "10.-#.23## #!?<5##>#!"#$!@<"##># %&'($)*+,-./,0$!"&$$!"1$ %2,3$,4,)5-*26)70$!"8$!;<=##>#!;<@##># 4#5# #! "10.-#.23##!"#$ %&'($)*+,-./,0$!"&$$ 6789(28:!;<=##># ν BG!?<5##>#!;<@##>#!@<"##># 33 止まっているK中間子を探すことになる Reduces atmospheric decay-electron tagging # # > 5.9 "10 years 5<G# (90% 55#&0:F 5<?# 5<*# 5<G#!;<=##># 5<G#!?<5##># 6789(28:!;<@##># CL)!@<"##># # #!!;<=##># 5<G#!?<5##># A.8&-'BC23#'.0( #DE!55#&0:F 5<?# 5<*# 6789(28:!; 33 ncy B Better decay-electron tagging + # > 5.9 "10 years A.8&-'BC23#'.0(#DE!55#&0:F p!" K 5<?# 5<*# 5<G# 5<G# (289()#.23#%.8&-'BC23#'.0()#.J('#.2.K:)9)#9/L'BM(/(20# SK-I+II+III+IV Preliminary # A.8&-'BC23#'.0( #DE!55#&0:F 5<?# 5<*#,III ~80% cf. SK-IV ~96% H(I#(789(289()#.23#%.8&-'BC23#'.0()#.J('#.2.K:)9)#9/L'BM(/(20# 酸素原子核中の陽子が崩壊したことによる励起 efficiency '(K9/92.':#Q5!?R#HB#8.2393.0()S#Q*5#&0B2#:'#DNO#!4Q4?4GFR# B p!" K + H(I#(789(289()#.23#%.8&-'BC23#'.0()#.J('#.2.K:)9)#9/L'BM(/(20# NCL('1O#P'(K9/92.':#Q5!?R#HB#8.2393.0()S#Q*5#&0B2#:'#DNO#!4Q4?4GFR# SK-I+II+III+ 0 ed particle ID and new π された窒素原子が出すガンマ線でタグ SK-I,II,III ~80% cf. SK-IV ~96% H(I#(789(289()#.23#%.8&-'BC23#'.0()#.J('#.2.K:)9)#9/ NCL('1O#P'(K9/92.':#Q5!?R#HB#8.2393.0()S#Q*5#&0B2#:'#DNO#!4Q4?4GFR# struction algorithm NCL('1O#P'(K9/92.':#Q5!?R#HB#8.2393.0()S#Q*5#&0B2#:'#DN 0 d π+π0 Refined particle ID and new π!"# SK-I SK-IIalgorithmSK-III reconstruction (20% coverage) SK-IV (new electronics)!"#!"#

lifetime (years) 10 36 10 35 10 34 10 33 M S = μ M 2 = 3 TeV M 16 = 1.0 10 GeV tanβ = 3 tanβ = 5 Hc tanβ = 10 tanβ = 30 tanβ = 50 10 2 10 3 10 4 10 5 M S (TeV) J. Hisano, D. Kobayashi, T. Kuwahara, N. Nagata (2013).

30»m B é» =»m W é» = 3 TeV,»m g é» = 10 TeV neutron Kaon EDM mixing 10 mæ3e tanb tanb 3 1 30 10 mæe conv. mæeg electron EDM charm mixing mæe conv. electron EDM neutron EDM Kaon mixing M h = 125.5±1 GeV 3 1 mæeg mæ3e charm mixing M h = 125.5±1 GeV 10 10 2 10 3 10 4 10 5 m q é = m l é =»m» HTeVL W. Altmannshofer, R. Harnik, J. Zupan, JHEP 1311 (2013) 202.

30»m B é» =»m W é» = 3 TeV,»m g é» = 10 TeV neutron Kaon EDM mixing 10 mæ3e tanb tanb 3 1 30 10 mæe conv. mæeg electron EDM charm mixing mæe conv. electron EDM neutron EDM Kaon mixing q i q j g q I M h = 125.5±1 GeV q J g q j q i 3 1 mæeg mæ3e charm mixing M h = 125.5±1 GeV 10 10 2 10 3 10 4 10 5 m q é = m l é =»m» HTeVL W. Altmannshofer, R. Harnik, J. Zupan, JHEP 1311 (2013) 202.

30»m B é» =»m W é» = 3 TeV,»m g é» = 10 TeV neutron Kaon EDM mixing 10 mæ3e tanb tanb 3 1 30 10 mæe conv. mæeg electron EDM charm mixing mæe conv. electron EDM neutron EDM Kaon mixing M h = 125.5±1 GeV g γ (g) 3 1 mæeg mæ3e u L charm mixing M h = 125.5±1 GeV 10 10 2 10 3 10 4 10 5 m q é = m l é =»m» HTeVL ũ L t L t R ũ R u R W. Altmannshofer, R. Harnik, J. Zupan, JHEP 1311 (2013) 202.

30»m B é» =»m W é» = 3 TeV,»m g é» = 10 TeV neutron Kaon EDM mixing 10 mæ3e tanb 3 1 30 10 mæe conv. tanb mæeg electron EDM charm mixing mæe conv. electron EDM neutron EDM Kaon mixing M h = 125.5±1 GeV 3 O(10 2 )TeV mæeg charm mixing 1 mæ3e M S M h = 125.5±1 GeV 10 10 2 10 3 10 4 10 5 m é q = m é T. Moroi and M. Nagai l =»m» (2013), HTeVL D. McKeen, M. Pospelov, A. Ritz (2013) W. Altmannshofer, R. Harnik, J. Zupan (2013), K. Fuyuto, J. Hisano, N. Nagata, K. Tsumura (2013) W. Altmannshofer, R. Harnik, J. Zupan, JHEP 1311 (2013) 202.

Ø Ø

Sfermion Flavor Viola+on ν µ,ν τ s t b u ũ δ Q L 13 g δ Q L 13 d d

10 37 10 36 10 35 1/Γ(p K + ν) [year] 10 34 10 33 10 32 10 31 10 30 δ Q L 13 δ Q L 12 M S = 100 TeV, M 1 = 600 GeV," M 2 = 300 GeV, M 3 = -2 TeV," μ = M S, M Hc = 10 16 GeV," tanβ = 5" 10 29 10 28 10 27 δũr 13 δ Q L 23 SK Limit 0.01 0.1 δ N. Nagata, S. Shirai (2013).

Minimal Flavor Violation 10 31 10 32 10 33 10 34 10 35 10 36 10 37 lifetime (years) 10 31 10 32 10 33 10 34 10 35 10 36 10 37 lifetime (years)

Soudan Frejus Kamiokande IMB Super-K p e + 0 n e + n + - p + 0 n + p + n 0 p e + p + n p e + 0 n e + n 0 p + 0 p + p e + p + n p e + K 0 n e + K - n e - K + p + K 0 n + K - p K + n K 0 p e + K*(892) 0 p K*(892) + n K*(892) 0 10 32 10 33 10 34 /B (years) 10 35 Super- Kamiokande

U i D j U k E l X X Q k L l Q i Q j

10 38 1/Γ(p π 0 µ + ) [year] 10 36 10 34 10 32 10 30 δ Q L 13 δ Q L 12 δũr 13 SK Limit M S = 100 TeV, M 1 = 600 GeV," M 2 = 300 GeV, M 3 = -2 TeV," μ = M S, M Hc = 10 16 GeV," tanβ = 5" 0.01 0.1 δ N. Nagata, S. Shirai (2013).

1 0.1 Uppuer bound 0.01 δ Q L 13 δ Q L 12 δ Q L 23 M S = 100 TeV, M 1 = 600 GeV," M 2 = 300 GeV, M 3 = -2 TeV," μ = M S, M Hc = 10 16 GeV," tanβ = 5" 0.001 10 1 10 2 10 3 10 4 m 0 [TeV] δũr 13 N. Nagata, S. Shirai (2013).

5. Conclusions and discussion

Discussion Ø Ø Ø Ø Ø

Summary

Backup

Minimal Flavor Viola+on

Sfermion Flavor Viola+on

-< 0 (ud) R u L p> < 0 (ud) L u L p> <K 0 (us) R u L p> <K 0 (us) L u L p> -<K + (us) R d L p> <K + (us) L d L p> -<K + (ud) R s L p> <K + (ud) L s L p> -<K + (ds) R u L p> -<K + (ds) L u L p> < (ud) R u L p> < (ud) L u L p> N f =2+1 "direct" N f =2+1 "indirect" 0 0.05 0.1 0.15 0.2 W 0 (µ=2gev) [GeV 2 ] Y. Aoki, E. Shintani, and A. Soni, arxiv:1304.7424

lifetime (years) 10 36 10 35 10 34 10 33 10 32 Super-Kamiokande Yukawa coupling Matrix element tan 10 M S = 100 TeV, M 1 = 600 GeV," M 2 = 300 GeV, M 3 = -2 TeV," μ = M S, M Hc = 10 16 GeV "

10 35 Γ 1 (p K + ν)[year] 10 34 10 33 10 32 Long-Distance Theory Short-Distance 0.01 0.1 δ Q L 13 N. Nagata, S. Shirai (2013).

s ν τ B s δ Q L 23 b ν τ t b δ Q L 13 δ Q L 13 ũ d g u d

ηµ + ηe + K + ν K 0 µ + K 0 e + π + ν M S = 100 TeV, M 1 = 600 GeV," M 2 = 300 GeV, M 3 = -2 TeV," μ = M S, M X = 10 16 GeV," tanβ = 5" π 0 µ + π 0 e + 10 30 10 32 10 34 10 36 10 38 10 40 Γ 1 [year]

10 37 M = 3 TeV 2 3 M S = 10 TeV lifetime (years) 10 36 10 35 10 34 10 33 10 1 M 3 (TeV)

10 9 8 7 Theory Experiment δ Q L 23 = δũr 23 =0.9 Q L 3 =4 tan β 6 5 4 3 2 1 10 1 10 2 10 3 10 4 10 5 m 0 [TeV] N. Nagata, S. Shirai (2013).

Dim- 5 proton decay via Planck suppressed operators 12 M scalar, no f mixing 11 m h excl tan 1 Log 10 MScalar GeV 10 9 8 m h excl tan 2 Hyper K p K excl Hyper K 7 p e excl 6 4 2 0 2 4 Log 10 M ino M Scalar M. Dine, P. Draper, W. Shepherd, arxiv: 1308.0274.

1 Uppuer bound 0.1 m 0 [TeV] d R 12 = QL 12 ũr 12 = Q L 12 d R 13 = QL 13 Q L 13 ũr 13 = 0.01 10 1 10 2 10 3 10 4 g γ (g) u L ũ L t L t R ũ R u R N. Nagata, S. Shirai (2013).

q i q I q j g g q j q J q i 1 1 0.1 Uppuer bound 0.1 δũr 13 = δũr 23 (D0 ) δ d R 13 (Bd 0) δ d R 23 (Bs) 0 0.01 10 1 10 2 10 3 10 4 m 0 [TeV] δ d R 12 (K 0 ) δũr 12 (D0 ) δ d R 13 = δ d R 23 (K 0 ) Uppuer bound 0.01 δũr 13 = δũr 23 = δ Q L 13 = δ Q L 23 (D0 ) δ d R 13 = δ Q L 13 (B0 d ) δ d R 23 = δ Q L 23 (B0 s) 0.001 10 1 10 2 10 3 10 4 m 0 [TeV] δ d R 12 = δ Q L 12 (K0 ) δũr 12 = δ Q L 12 (D0 ) δ d R 13 = δ d R 23 = δ Q L 13 = δ Q L 23 (K0 ) N. Nagata, S. Shirai (2013).