Phenomenological Status of Neutrino Mixing
|
|
|
- Arleen Malone
- 6 years ago
- Views:
Transcription
1 Phenomenological Status of Neutrino Mixing Carlo Giunti INFN, Sezione di Torino, and Dipartimento di Fisica Teorica, Università di Torino Neutrino Unbound: SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre 007 C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre 007 1
2 Outline Brief Introduction on Neutrino Masses Solar Neutrinos and KamLAND Atmospheric Neutrinos, KK and MINOS Three-Neutrino Mixing Absolute Scale of Neutrino Masses Tritium Beta-Decay Neutrinoless Double-Beta Decay Cosmology LSND and MiniBooNE Conclusions C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre 007
3 Standard Model: Massless Neutrinos ÓÓ Ø Ä Ô Î Ú Ô ¼ Ê Ú Ô Standard Model: L c L = (c ) R =µ no Dirac mass term Majorana Neutrino: c Ä D m D L R (no R, ( c ) L ) ( c ) R R =µ Majorana mass term Ä M m M L c L = m M L ( c ) R Standard Model: Majorana mass term not allowed by SU() L U(1) Y (no Higgs triplet) C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre 007 3
4 Extension of the SM: Massive Neutrinos Standard Model can be extended with R (e L e R ; u L u R ; d L d R ; ) L + R µ Dirac neutrino mass term Ä D m D L R µ m D 100 GeV surprise: Majorana neutrino mass for R is allowed! total neutrino mass term Ä D+M L ( c ) L 0 m D m D Ä M R mm R (c ) L R m M R ( c ) R R m M R can be arbitrarily large (not protected by SM symmetries) mr M scale of new physics beyond Standard Model µ mm R md 0 m D diagonalization of µ m 1 ³ (md ), m ³ mr M ν ν 1 see-saw mechanism m D m M R m M R natural explanation of smallness of neutrino masses massive neutrinos are Majorana! [Minkowski, PLB 67 (1977) 4] [Yanagida (1979); Gell-Mann, Ramond, Slansky (1979); Mohapatra, Senjanovic, PRL 44 (1980) 91] C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre 007 4
5 Lepton Numbers Standard Model: Lepton numbers are conserved L e L L ( e e ) ( ) ( ) L e L L (( c ) e e + ) (( c ) + ) (( c ) + ) L = L e + L + L ¼ ½¼ md ee m D e m D e er Dirac mass term m D L R el L L me D m D m D R me D m D m D R L e, L, L are not conserved, but L is conserved L( «R) = L( L) µ L = 0 Majorana mass term m M L ( c ) R el L L ¼ ½¼ mm ee m M e m M e me M mm mm me M m M m M L, L e, L, L are not conserved L( c «) = L( ) µ L = ½ (c e ) R () c R ( c ) R ½ C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre 007 5
6 «= U = Two-Neutrino Mixing and Oscillations k=1 cos sin U «k k («= e ) sin cos ν µ ν ϑ ν e ν 1 e = cos 1 + sin = sin 1 + cos m m 1 m m 1 Transition Probability: P e = P e = sin sin m L 4E Survival Probabilities: P ee = P = 1 P e C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre 007 6
7 Solar Neutrinos Solar e Energy Spectrum [J.N. Bahcall, C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre 007 7
8 Homestake+Kam.+GALLEX+SAGE+Super-K+SNO 6 Φ SNO e = cm s 1 Φ SNO e = cm s 1 SNO solved solar neutrino problem Neutrino Physics (April 00) [SNO, PRL 89 (00) , nucl-ex/004008] e oscillations LMA: Large Mixing Angle solution m ³ ev tan ³ s -1 ) cm - 10 ( φ µτ SNO φcc 68% C.L. SNO φnc 68% C.L. SNO φes 68% C.L. SK φes 68% C.L. BS05 φssm 68% C.L. NC φµτ 68%, 95%, 99% C.L φ ( 10 cm - s -1 e ) ) ev -5 (10 m (a) tan θ [SNO, PRC 7 (005) 05550, nucl-ex/05001] C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre 007 8
9 BOREXino [BOREXino, arxiv: ] Real-time measurement of 7 Be solar neutrinos (086MeV) + e + e E = 086MeV =µ e ³ 55 Counts/(10 kev day 100 tons) All solar neutrinos 7 Be neutrinos Energy [MeV] Counts/(10 kev day 100 tons) Fit: χ /NDF = 41.9/47 7 Be: 47±7±1 cpd/100 tons 10 Bi+CNO: 15±4±5 cpd/100 tons 85 Kr: ±7±5 cpd/100 tons 10 Po: 0.9±1. cpd/100 tons Energy [kev] n no-osc the = 75 4day 1 (100tons) 1 n exp = day 1 (100tons) 1 n osc the = 49 4day 1 (100tons) 1 (n no-osc the n exp ) n ³ 19 C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre 007 9
10 KamLAND Reactor e e confirmation of LMA (December 00) 53 nuclear power reactors in Japan and Korea Kamioka Mine L ³ 180km E ³ 4MeV short baseline experiment Ratio 1.4 KamLAND data CHOOZ data best-fit osci. 1. best-fit osci. + Expected Geo e st nd 3rd preliminary L 0 /E e (km/mev) [I. Shimizu (KamLAND), TAUP 007] hypothetical single reactor at 180 km C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre
11 ) (ev m small matter effect SNO KamLAND KamLAND 95% C.L. 99% C.L % C.L. best fit SNO 95% C.L. 99% C.L % C.L. best fit tan 4 3 preliminary > 6 > 4 KamLAND only tan = 0.56 m = ev LMA II LMA 0 [I. Shimizu (KamLAND), TAUP 007] (marginalized error) ) ev -5 (10 m neutrino effect 3 neutino neutino preliminary sin 1 same result for m C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre
12 ) (ev KamLAND tan = KamLAND + Solar % C.L. 99% C.L % C.L. 0.3 global best fit m = ev This result KamLAND + SNO tan = m = ev m : systematic uncertainty.0% dominated by linear energy scale uncertainty m tan ev ) -5 (10 m 7 6 preliminary KamLAND + SNO 95% C.L. 99% C.L % C.L. best fit tan m is measured at.8% precision by KamLAND [I. Shimizu (KamLAND), TAUP 007] C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre 007 1
13 Atmospheric Neutrinos e + νe νµ π + p π µ + µ νµ νµ νµ νe e N( + ) N( e + e ) ³ at E 1GeV uncertainty on ratios: 5% uncertainty on fluxes: 30% ratio of ratios dn/dlne, (Kt.yr) sub GeV multi GeV stopping muons through-going muons E ν, GeV (m.yr.ster) -1 R [N( + )N( e + e )] data [N( + )N( e + e )] MC R K sub-gev R K multi-gev = [Kamiokande, PLB 80 (199) 146] = [Kamiokande, PLB 335 (1994) 37] C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre
14 Super-Kamiokande Up-Down Asymmetry A θ AB z E 1GeV µ isotropic flux of cosmic rays ν α B (A) «( AB z ) = (B) «( AB z ) (A) «(A) «( z ) = (A) ( AB z «( z ) ) = (B) «(z AB ) π θ AB z up N A up-down (SK) = (December 1998) N down N up + N down = [Super-Kamiokande, Phys. Rev. Lett. 81 (1998) 156, hep-ex/ ] 6 MODEL INDEPENDENT EVIDENCE OF DISAPPEARANCE! C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre
15 Fit of Super-Kamiokande Atmospheric Data 10 - Measure of CC Int. is Difficult: E th = 35 GeV =µ 0eventsyr -Decay =µ Many Final States m (ev ) 10-3 Best Fit: 99% C.L. 90% C.L. 68% C.L sin θ m = ev sin = live-days (Apr 1996 Jul 001) [Super-Kamiokande, PRD 71 (005) 11005, hep-ex/ ] -Enriched Sample N the = 78 m = ev N exp = N 4 [Super-Kamiokande, PRL 97(006) , hep-ex/ ] Future Check: OPERA ( ) CERN to Gran Sasso (CNGS) L ³ 73 km E ³ 18 GeV [NJP 8 (006) 303, hep-ex/061103] C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre
16 Kamiokande, Soudan-, MACRO and MINOS m (ev ) Kamiokande up µ 90%CL CDHSW 10 - Kamiokande contained 10-3 Kamiokande up µ 95%CL Kamiokande contained + up µ sin θ [Kamiokande, PRL 81 (1998) 016, hep-ex/ ] [Soudan, PRD 7 (005) 05005, hep-ex/ ] m (ev ) 10-1: Angular distribution : Energy(Low/High) 1+ m (ev ) % C.L. 90 % C.L. - lnl=.3 Best fit MINOS Atmospheric ν 418 days exposure sin θ [MACRO, PLB 566 (003) 35, hep-ex/ ] sin θ [MINOS, PRD 73 (006) 0700, hep-ex/051036] C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre
17 KK KEK to Kamioka (Super-Kamiokande) L ³ 50km E ³ 13GeV confirmation of atmospheric allowed region (June 00) events/0.gev m [10-3 ev ] rec E ν GeV 1 KK 68% KK 90% KK 99% SK L/E 90% sin (θ) best fit: m = ev sin = 100 [KK, PRD 74 (006) 07003, hep-ex/060603] C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre
![MINOS Fermilab to Soudan Mine (Minnesota) L ³ 730km E ³ 35GeV [MINOS, TAUP 007]](/docs-images/73/68854481/images/18-0.jpg "C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre 007")
18 MINOS Fermilab to Soudan Mine (Minnesota) L ³ 730km E ³ 35GeV [MINOS, TAUP 007] C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre
19 Experimental Evidences of Neutrino Oscillations Solar e Reactor e disappearance Atmospheric Accelerator disappearance ¼ ¼ Homestake Kamiokande/Super-K GALLEX/GNO SAGE Super-Kamiokande SNO BOREXino (KamLAND) Kamiokande IMB Super-Kamiokande MACRO Soudan- (KK & MINOS) ½ ½ m SUN = 759 (1 003) 10 5 ev sin SUN = [I. Shimizu (KamLAND), TAUP 007] matm = ev sin ATM = [Fogli et al, PRD 75 (007) , hep-ph/ ] C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre
20 Three-Neutrino Mixing «L = 3 k=1 U «k kl («= e ) three flavor fields e,, three massive fields 1,, 3 m SUN = m 1 ³ ev m ATM ³ m 31 ³ m 3 ³ ev C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre 007 0
21 Allowed Three-Neutrino Schemes Ñ Ñ ¾ ËÍÆ Ñ ¾ ½ Ñ ¾ ÌÅ Ñ ¾ ÌÅ ¾ Ñ ¾ ËÍÆ ½ normal inverted different signs of m 31 ³ m 3 absolute scale is not determined by neutrino oscillation data C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre 007 1
22 Mixing Matrix ËÍÆ Í ½ Í ¾ Í δm (ev ) 1 Analysis A ν e ν x 90% CL Kamiokande (multi-gev) m 1 m 31 Í Í ½ Í ¾ Í % CL Kamiokande (sub+multi-gev) Í ½ Í ¾ Í ÌÅ 10 - CHOOZ: m CHOOZ = m 31 = m ATM sin CHOOZ = 4U e3 (1 U e3 ) U e for m 10 ev % CL 95% CL SOLAR AND ATMOSPHERIC OSCILLATIONS ARE PRACTICALLY DECOUPLED! sin (θ) [CHOOZ, PLB 466 (1999) 415] see also [Palo Verde, PRD 64 (001) 11001] TWO-NEUTRINO SOLAR and ATMOSPHERIC OSCILLATIONS ARE OK! sin SUN = U e 1 U e3 ³ U e sin ATM = U 3 [Bilenky, C.G, PLB 444 (1998) 379] [Guo, Xing, PRD 67 (003) 05300] C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre 007
23 Standard Parameterization of Mixing Matrix ¼ U = c 3 s 3 0 s 3 c 3 = ¼ 3 ³ ATM ¼ el L L ½¼ ½ ¼ = U e1 U e U e3 U 1 U U 3 U 1 U U 3 c 13 0 s 13 e i Æ s 13 e i Æ13 0 c = CHOOZ ½¼ ½¼ 1L L 3L ½ c 1 s 1 0 s 1 c ³ SUN c 1c 13 s 1c 13 s 13e i Æ 13 s 1c 3 c 1s 3s 13e i Æ 13 c 1c 3 s 1s 3s 13e i Æ 13 s 3c 13 s 1s 3 c 1c 3s 13e i Æ 13 c 1s 3 s 1c 3s 13e i Æ 13 c 3c 13 ½¼ ½¼ e i e i e i e i 3 0 ½ ½ C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre 007 3
24 Global Fit of Oscillation Data: Bilarge Mixing 10 m 1 [10-5 ev ] tan θ 1 sin θ 13 4 m 31 [10-3 ev ] tan θ 3 sin θ 13 [Gonzalez-Garcia, Maltoni, arxiv: ] C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre 007 4
25 m 1 = m ev = 6 0(06) 10 3 ev ¼ U 90% = ¼ U 3 = 1 = = = ½ ½ [Gonzalez-Garcia, Maltoni, arxiv: ] future: measure 13 = 0 =µ CP violation, matter effects, mass hierarchy C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre 007 5
26 Absolute Scale of Neutrino Masses normal scheme inverted scheme 10 0 QUASI DEGENERATE 10 0 QUASI DEGENERATE 10 1 m m m1 m [ev ] 10 m m [ev ] m1 NORMAL SCHEME 10 3 m3 INVERTED SCHEME NORMAL HIERARCHY Lightest Mass: m1 [ev ] INVERTED HIERARCHY Lightest Mass: m3 [ev ] 10 0 m = m 1 + m 1 = m 1 + m SUN m 3 = m 1 + m 31 = m 1 + m ATM m 1 = m 3 m 31 = m 3 + m ATM m = m 1 + m 1 ³ m 3 + m ATM Quasi-Degenerate for m 1 ³ m ³ m 3 ³ m Ô m ATM ³ 5 10 ev C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre 007 6
27 3 H 3 He + e + e Tritium Beta-Decay Õ dγ dt = (coscgf) Å F(E)pE (Q T) (Q T) m 3 e Q = M3 H M3 He m e = 1858keV m e = m = k U ek m k K(T) = ÚÙ Ù Ø 3 Kurie plot dγdt = (coscg F) Å F(E)pE (Q T) Õ 1 (Q T) m e K(T) m νe = m νe = 100 ev T Q m νe Q m e ev (95% C.L.) Mainz & Troitsk [Weinheimer, hep-ex/010050] future: KATRIN (start 010) [hep-ex/ ] [hep-ex/ ] sensitivity: m e ³ 0eV C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre 007 7
28 m e = m = U e1 m 1 + U e m + U e3 m NORMAL SCHEME 10 1 INVERTED SCHEME 10 0 Mainz & Troitsk 10 0 Mainz & Troitsk mβ [ev ] 10 1 m3 KATRIN mβ [ev ] 10 1 m1,m KATRIN 10 m 10 m1 m Lightest Mass: m 1 [ev ] Quasi-Degenerate: m 1 ³ m ³ m 3 ³ m =µ m ³ m Lightest Mass: m 3 [ev ] k U ek = m FUTURE: IF m 4 10 ev =µ NORMAL HIERARCHY C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre 007 8
29 Neutrinoless Double-Beta Decay + β As 0 + β 76 3Ge β β Se C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre 007 9
30 Two-Neutrino Double- Decay: L = 0 Æ(A Z) Æ(A Z + ) + e + e + e + e Ï Ù (T 1 ) 1 = G Å second order weak interaction process in the Standard Model Ï Ù Neutrinoless Double- Decay: L = Æ(AZ) Æ(AZ + ) + e + e (T 0 1 ) 1 = G 0 Å 0 m Ï Í Ù effective Majorana mass m = k U ek m k Ñ Í Ï Ù C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre
31 Majorana Neutrino Mass? ν 1 ν ν 3 u d s e µ c b τ t m [ev] known natural explanation of smallness of masses New High Energy Scale Å µ both imply See-Saw Mechanism (if R s exist) 5-D Non-Renormaliz. Eff. Operator Majorana masses µ L = µ 0 see-saw type relation m Å EW Å Majorana neutrino masses provide the most accessible window on New Physics Beyond the Standard Model decay C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre
32 Effective Majorana Neutrino Mass m = k U ek m k complex U ek µ possible cancellations m = U e1 m 1 + U e e i «m + U e3 e i «3 m 3 «= «3 = ( 3 Æ 13 ) Im[m ββ ] m ββ U e3 e iα 3 m 3 U e e iα m U e1 m 1 Re[m ββ ] C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre 007 3
33 Experimental Bounds T y T y Heidelberg-Moscow ( 76 Ge) [EPJA 1 (001) 147] T y T y (90% C.L.) =µ m 03 10eV IGEX ( 76 Ge) [PRD 65 (00) 09007] (90% C.L.) =µ m eV CUORICINO ( 130 Te) [PRL 95 (005) 14501] (90% C.L.) =µ m 0 11eV NEMO 3 ( 100 Mo) [PRL 95 (005) 1830] (90% C.L.) =µ m 07 8eV FUTURE EXPERIMENTS CAMEO, CANDLES, COBRA, EXO, Majorana, XMASS m few10 1 ev CUORE, MOON, GEM, GERDA, SNO++, Super-NEMO m few10 ev C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre
34 Bounds from Neutrino Oscillations m = U e1 m 1 + U e e i «m + U e3 e i «3 m NORMAL SCHEME 10 1 INVERTED SCHEME mββ [ev] EXP CP violation mββ [ev] EXP CP violation LightestMass: m 1 [ev] LightestMass: m 3 [ev] 10 1 FUTURE: IF m 10 ev =µ NORMAL HIERARCHY C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre
35 Experimental Positive Indication [Klapdor et al., MPLA 16 (001) 409] T 0 1 = ( ) 105 y 65 evidence [MPLA 1 (006) 1547] Counts / kev SSE nb Rosen Primakov Approximation Q=039 kev Energy,keV [PLB 586 (004) 198] [MPLA 1 (006) 1547] the indication must be checked by other experiments m = eV [MPLA 1 (006) 1547] if confirmed, very exciting (Majorana and large mass scale) C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre
36 Cosmology H 0 (Hubble Space Telescope Key Project) CMBR (COBE, WMAP, Boomerang, DASI, MAXIMA, VSA, CBI, ACBAR) LSS (dfgrs, SDSS) SNIa (High-z SN Search Team, Supernova Cosmology Project) ΛCDM =µ 3 k=1 m k 0 07eV C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre
37 LSND and MiniBooNE m (ev /c 4 ) e Karmen Bugey CCFR NOMAD ) 4 /c (ev m 10 1 e MiniBooNE 90% C.L.y KARMEN 90% C.L. Bugey 90% C.L % (L max -L <.3) 99% (L max -L < 4.6) sin θ [LSND, PRD 64 (001) 11007, hep-ex/ ] m LSND 01eV LSND 90% C.L. LSND 99% C.L sin (θ) [MiniBooNE, PRL 98 (007) 31801, arxiv: ] e is running m LSND m ATM m SUN C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre
38 MiniBooNE Low-Energy Anomaly events / MeV ν oscillation analysis threshold MiniBooNE datay expected backgroundgν µ BG + best-fit ν µ ν e ν µ background ν µ background ν e 0.5 excess events / MeV data - expected background best-fit ν µ ν e sin (θ)=0.004, m =1.0 ev sin (θ)=0., m =0.1 ev ν µ ν µ reconstructed E ν (MeV) [MiniBooNE, PRL 98 (007) 31801, arxiv: ] C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre
39 Conclusions e with msun ³ ev (solar, KamLAND) with matm ³ ev (atm., KK, MINOS) Bilarge 3-Mixing with U e3 1 (CHOOZ) Decay, Cosmology, 0 Decay =µ m 1eV Exp.: Theory: FUTURE Why lepton mixing = quark mixing? Why only U e3 1? Improve calculation of Å 0! LSND and MiniBooNE Low-Energy Anomaly? Measure U e3 0 µ CP violation, matter eff., mass hierarchy Check 0 signal at Quasi-Degenerate mass scale Improve Decay, Cosmology, 0 Decay measurements LSND and MiniBooNE Low-Energy Anomaly? C. Giunti Neutrino Mixing SIF, XCIII Congresso Nazionale, Pisa, 5 Settembre
Neutrino Mass: Overview of ββ 0ν, Cosmology and Direct Measurements Carlo Giunti
Neutrino Mass: Overview of ββ 0ν, Cosmology and Direct Measurements Carlo Giunti INFN, Sezione di Torino, and Dipartimento di Fisica Teorica, Università di Torino mailto://giunti@to.infn.it Neutrino Unbound:
Carlo Giunti. CERN Particle and Astro-Particle Physics Seminar. work in collaboration with Mario Acero Marco Laveder Walter Winter
Very-Short-BaseLine Electron Neutrino Disappearance Carlo Giunti INFN, Sezione di Torino, and Dipartimento di Fisica Teorica, Università di Torino mailto://giunti@to.infn.it Neutrino Unbound: http://www.nu.to.infn.it
Sterile Neutrinos in July 2010
Sterile Neutrinos in July 0 Carlo Giunti INFN, Sezione di Torino Presidenza INFN, Roma, 19 July 0 Collaboration with Marco Laveder (Padova University) C. Giunti Sterile Neutrinos in July 0 Presidenza INFN,
Neutrino Masses in Cosmology, Neutrinoless Double-Beta Decay and Direct Neutrino Masses Carlo Giunti
Neutrino Masses in Cosmology, Neutrinoless Double-Beta Decay and Direct Neutrino Masses Carlo Giunti INFN, Sezione di Torino, and Dipartimento di Fisica Teorica, Università di Torino mailto://giunti@to.infn.it
Neutrino Physics II. Neutrino Phenomenology. Arcadi Santamaria. TAE 2014, Benasque, September 19, IFIC/Univ. València
Neutrino Physics II Neutrino Phenomenology Arcadi Santamaria IFIC/Univ. València TAE 2014, Benasque, September 19, 2014 Neutrino Physics II Outline 1 Neutrino oscillations phenomenology Solar neutrinos
Neutrino Physics. Carlo Giunti
Neutrino Physics Carlo Giunti INFN, Sezione di Torino, and Dipartimento di Fisica Teorica, Università di Torino mailto://giunti@to.infn.it Neutrino Unbound: http://www.nu.to.infn.it CERN, 12 15 May 2009
Status of Light Sterile Neutrinos Carlo Giunti
C. Giunti Status of Light Sterile Neutrinos EPS-HEP 05 3 July 05 /5 Status of Light Sterile Neutrinos Carlo Giunti INFN, Sezione di Torino and Dipartimento di Fisica, Università di Torino giunti@to.infn.it
Sterile Neutrinos. Carlo Giunti
C. Giunti Sterile Neutrinos PPC07 6 May 07 /5 Sterile Neutrinos Carlo Giunti INFN, Torino, Italy XI International Conference on Interconnections between Particle Physics and Cosmology Corpus Christi, Texas,
Status of Light Sterile Neutrinos Carlo Giunti
Status of Light Sterile Neutrinos Carlo Giunti INFN, Torino, Italy EPS-HEP 07 07 European Physical Society Conference on High Energy Physics Venezia, Italy, 5- July 07 C. Giunti Status of Light Sterile
Neutrino oscillation experiments: Recent results and implications
Title transparency Neutrino oscillation experiments: Recent results and implications W. Hampel MPI Kernphysik Heidelberg Motivation for talk On the way from the Standard Model to String Theory: appropriate
Neutrino Experiments: Lecture 2 M. Shaevitz Columbia University
Neutrino Experiments: Lecture 2 M. Shaevitz Columbia University 1 Outline 2 Lecture 1: Experimental Neutrino Physics Neutrino Physics and Interactions Neutrino Mass Experiments Neutrino Sources/Beams and
Neutrino Oscillation Measurements, Past and Present. Art McDonald Queen s University And SNOLAB
Neutrino Oscillation Measurements, Past and Present Art McDonald Queen s University And SNOLAB Early Neutrino Oscillation History -1940 s to 1960 s: - Neutrino oscillations were proposed by Pontecorvo
NEUTRINOS II The Sequel
NEUTRINOS II The Sequel More About Neutrinos Ed Kearns Boston University NEPPSR V - 2006 August 18, 2006 Ed Kearns Boston University NEPPSR 2006 1 There is something unusual about this neutrino talk compared
Neutrino Oscillations
Neutrino Oscillations Heidi Schellman June 6, 2000 Lots of help from Janet Conrad Charge mass,mev tandard Model of Elementary Particles 3 Generations of Fermions Force Carriers Q u a r k s u d 2/3 2/3
Unbound Neutrino Roadmaps. MARCO LAVEDER Università di Padova e INFN NOW September 2006
Unbound Neutrino Roadmaps MARCO LAVEDER Università di Padova e INFN NOW 2006-11 September 2006 Experimental Data : 2006 Experiment Observable (# Data) Measured/SM Chlorine Average Rate (1) [CC]=0.30 ±
Neutrinos and Cosmos. Hitoshi Murayama (Berkeley) Texas Conference at Stanford Dec 17, 2004
Neutrinos and Cosmos Hitoshi Murayama (Berkeley) Texas Conference at Stanford Dec 17, 2004 Outline A Little Historical Perspective Interpretation of Data & Seven Questions Matter Anti-Matter Asymmetry
Oscillations Beyond Three-Neutrino Mixing (Status of Light Sterile Neutrinos) Carlo Giunti
C. Giunti Oscillations Beyond Three-Neutrino Mixing Moriond EW 07 4 March 07 /3 Oscillations Beyond Three-Neutrino Mixing (Status of Light Sterile Neutrinos) Carlo Giunti INFN, Torino, Italy Moriond Electroweak
Neutrino physics. Evgeny Akhmedov. Max-Planck-Institut für Kernphysik, Heidelberg & Kurchatov Institute, Moscow
Neutrino physics Experimental results and future Evgeny Akhmedov Max-Planck-Institut für Kernphysik, Heidelberg & Kurchatov Institute, Moscow Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct.
Neutrino Basics. m 2 [ev 2 ] tan 2 θ. Reference: The Standard Model and Beyond, CRC Press. Paul Langacker (IAS) LSND 90/99% SuperK 90/99% MINOS K2K
![Neutrino Basics. m 2 [ev 2 ] tan 2 θ. Reference: The Standard Model and Beyond, CRC Press. Paul Langacker (IAS) LSND 90/99% SuperK 90/99% MINOS K2K](/thumbs/93/112869275.jpg "Neutrino Basics. m 2 [ev 2 ] tan 2 θ. Reference: The Standard Model and Beyond, CRC Press. Paul Langacker (IAS) LSND 90/99% SuperK 90/99% MINOS K2K")
Neutrino Basics CDHSW m 2 [ev 2 ] 10 0 10 3 10 6 10 9 KARMEN2 Cl 95% NOMAD MiniBooNE Ga 95% Bugey CHOOZ ν X ν µ ν τ ν τ NOMAD all solar 95% SNO 95% CHORUS NOMAD CHORUS LSND 90/99% SuperK 90/99% MINOS K2K
Status of neutrino mass-mixing parameters and implications for single and double beta decay searches
Padova, 24 febbraio 2007 Status of neutrino mass-mixing parameters and implications for single and double beta decay searches Gianluigi Fogli Dipartimento di Fisica dell Università di Bari & Sezione INFN
Solar and atmospheric ν s
Solar and atmospheric ν s Masato SHIOZAWA Kamioka Observatory, Institute for Cosmic Ray Research, U of Tokyo, and Kamioka Satellite, Kavli Institute for the Physics and Mathematics of the Universe (WPI),
Recent Discoveries in Neutrino Oscillation Physics & Prospects for the Future
Recent Discoveries in Neutrino Oscillation Physics & Prospects for the Future Karsten M. Heeger Lawrence Berkeley National Laboratory 8 7 6 5 4 3 2 1 SNO φ ES SNO φ CC SNO φ NC SSM φ NC 0 0 1 2 3 4 5 6
1 Neutrinos. 1.1 Introduction
1 Neutrinos 1.1 Introduction It was a desperate attempt to rescue energy and angular momentum conservation in beta decay when Wolfgang Pauli postulated the existence of a new elusive particle, the neutrino.
Oscillations Beyond Three-Neutrino Mixing. Carlo Giunti
C. Giunti Oscillations Beyond Three-Neutrino Mixing CNNP07 9 October 07 /3 Oscillations Beyond Three-Neutrino Mixing Carlo Giunti INFN, Torino, Italy CNNP07 Conference on Neutrino and Nuclear Physics Catania,
Hint of CPT Violation in Short-Baseline Electron Neutrino Disappearance
Journal of Physics: Conference Series 335 (011) 01054 doi:10.1088/174-6596/335/1/01054 Hint of CPT Violation in Short-Baseline Electron Neutrino Disappearance Carlo Giunti INFN, Sezione di Torino, and
Particle Physics: Neutrinos part II
Particle Physics: Neutrinos part II José I. Crespo-Anadón Week 9: April 1, 2017 Columbia University Science Honors Program Course Policies Attendance Up to four absences Send email notifications of all
March 30, 01 Lecture 5 of 6 @ ORICL Philosophical Society Yuri Kamyshkov/ University of Tennessee email: kamyshkov@utk.edu 1. Concept/misconception of mass in Special Relativity (March,9). and n Oscillations:
Neutrinos as a Unique Probe: cm
Neutrinos as a Unique Probe: 10 33 10 +28 cm Particle Physics νn, µn, en scattering: existence/properties of quarks, QCD Weak decays (n pe ν e, µ e ν µ ν e ): Fermi theory, parity violation, quark mixing
Introduction to Neutrino Physics
Introduction to Neutrino Physics Tommy Ohlsson tommy@theophys.kth.se Royal Institute of Technology (KTH) Stockholm Center for Physics, Astronomy, and Biotechnology Stockholm, Sweden Abisko, Norrbotten,
What We Know, and What We Would Like To Find Out. Boris Kayser Minnesota October 23,
What We Know, and What We Would Like To Find Out Boris Kayser Minnesota October 23, 2008 1 In the last decade, observations of neutrino oscillation have established that Neutrinos have nonzero masses and
Neutrinos as Probes of new Physics
Neutrinos as Probes of new Physics Manfred Lindner Max-Planck-Institut für Kernphysik, Heidelberg The Birth of the Neutrino energy-momentum conservation: postulate new particle invisible, since Q=0 spin
On Minimal Models with Light Sterile Neutrinos
On Minimal Models with Light Sterile Neutrinos Pilar Hernández University of Valencia/IFIC Donini, López-Pavón, PH, Maltoni arxiv:1106.0064 Donini, López-Pavón, PH, Maltoni, Schwetz arxiv:1205.5230 SM
SNOW Global fits to neutrino oscillation data. Thomas Schwetz SISSA, Trieste
SNOW 26 Global fits to neutrino oscillation data Thomas Schwetz SISSA, Trieste based on work in collaboration with M. Maltoni, M.A. Tortola, and J.W.F. Valle [hep-ph/3913, hep-ph/45172] T.S. is supported
1. Neutrino Oscillations
Neutrino oscillations and masses 1. Neutrino oscillations 2. Atmospheric neutrinos 3. Solar neutrinos, MSW effect 4. Reactor neutrinos 5. Accelerator neutrinos 6. Neutrino masses, double beta decay 1.
Updating the Status of Neutrino Physics
Updating the Status of Neutrino Physics J. W. F. Valle IFIC-CSIC/U. Valencia Based on hep-ph/36 and hep-ph/3792 String Phenomenology 23, Durham p. Atmospheric zenith distribution Maltoni, Schwetz, Tortola
Neutrinos. Thanks to Ian Blockland and Randy Sobie for these slides. spin particle with no electric charge; weak isospin partners of charged leptons
Neutrinos Thanks to Ian Blockland and Randy Sobie for these slides spin particle with no electric charge; weak isospin partners of charged leptons observed in 193, in 1962 and in the 199s neutrino physics
Neutrino Physics: Lecture 12
Neutrino Physics: Lecture 12 Sterile neutrinos Amol Dighe Department of Theoretical Physics Tata Institute of Fundamental Research Apr 5, 2010 Outline 1 Short baseline experiments and LSND anomaly 2 Adding
Sterile Neutrino Searches: Experiment and Theory Carlo Giunti INFN, Sezione di Torino
C. Giunti Sterile Neutrino Searches Tau06 Sep 06 /3 Sterile Neutrino Searches: Experiment and Theory Carlo Giunti INFN, Sezione di Torino Tau06 4th International Workshop on Tau Lepton Physics 9-3 September
Short-Baseline Neutrino Oscillation Anomalies and Light Sterile Neutrinos. Carlo Giunti
C. Giunti SBL Neutrino Oscillation Anomalies and Light Sterile Neutrinos Roma Tre Nov 07 /53 Short-Baseline Neutrino Oscillation Anomalies and Light Sterile Neutrinos Carlo Giunti INFN, Torino, Italy Seminar
The Effect of Cancellation in Neutrinoless Double Beta Decay
The Effect of Cancellation in Neutrinoless Double Beta Decay Manimala Mitra IPPP, Durham University July 24, 204 SUSY 204, Manchester arxiv:30.628, Manimala Mitra, Silvia Pascoli, Steven Wong Manimala
C. Giunti Sterile Neutrino Mixing NOW Sep /25
Sterile Neutrino Mixing NOW and in the Next Years Carlo Giunti INFN, Sezione di Torino NOW 06 Neutrino Oscillation Workshop 4- September 06 Otranto, Lecce, Italy C. Giunti Sterile Neutrino Mixing NOW 06
The future of neutrino physics (at accelerators)
Mauro Mezzetto, Istituto Nazionale Fisica Nucleare, Padova The future of neutrino physics (at accelerators) Present Status Concepts, strategies, challenges The two players: Dune and Hyper-Kamiokande Conclusions
Neutrino mixing II. Can ν e ν µ ν τ? If this happens:
Can ν e ν µ ν τ? If this happens: Neutrino mixing II neutrinos have mass (though there are some subtleties involving the MSW mechanism) physics beyond the (perturbative) Standard Model participates Outline:
Solar Neutrino Road Map. Carlos Pena Garay IAS
α Solar Neutrino Road Map Carlos Pena Garay IAS ~ February 11, 004 NOON004 Be + p-p p p (pep) measurements Why perform low-energy solar neutrino experiments? Amazing progress on how the Sun shines, the
Neutrino Oscillations
1. Introduction 2. Status and Prospects A. Solar Neutrinos B. Atmospheric Neutrinos C. LSND Experiment D. High-Mass Neutrinos 3. Conclusions Plenary talk given at DPF 99 UCLA, January 9, 1999 Introduction
Status of the Sterile Neutrino(s) Carlo Giunti
C. Giunti Status of the Sterile Neutrino(s) LNGS 7 September 07 /40 Status of the Sterile Neutrino(s) Carlo Giunti INFN, Torino, Italy Recent Developments in Neutrino Physics and Astrophysics th Anniversary
Neutrino Oscillations
Neutrino Oscillations Elisa Bernardini Deutsches Elektronen-Synchrotron DESY (Zeuthen) Suggested reading: C. Giunti and C.W. Kim, Fundamentals of Neutrino Physics and Astrophysics, Oxford University Press
Review of Neutrino Oscillation Experiments
Flavor Physics and CP Violation Conference, Vancouver, Review of Neutrino Oscillation Experiments M.D. Messier Department of Physics, Indiana University, Bloomington IN, 4745, USA Several experiments have
Sensitivity to sterile ν mixings at a ν Factory --Side business of a ν Factory --
Sensitivity to sterile ν mixings at a ν Factory --Side business of a ν Factory -- Osamu Yasuda Tokyo Metropolitan University 009-1-18 @ Miami009 1 1. Introduction. Light sterile neutrinos 3. Summary 1.
MINOS Result. The ND analysis predicts: events in the Far Detector 54 observed, 0.7σ excess. 49.1±7.0(stat.)±2.7(syst.
MINOS Result The ND analysis predicts: 49.1±7.0(stat.)±2.7(syst.) events in the Far Detector 54 observed, 0.7σ excess 26 MINOS Result The ND analysis predicts: 49.1±7.0(stat.)±2.7(syst.) events in the
Sterile neutrinos. Stéphane Lavignac (IPhT Saclay)
Sterile neutrinos Stéphane Lavignac (IPhT Saclay) introduction active-sterile mixing and oscillations cosmological constraints experimental situation and fits implications for beta and double beta decays
Status of Neutrino Masses and Mixing
Status of Neutrino Masses and Mixing Carlo Giunti INFN, Sezione di Torino, and Dipartimento di Fisica Teorica, Università di Torino giunti@to.infn.it POSTECH, Pohang, Korea, October 004 Introduction to
Neutrinos: status, models, string theory expectations
Neutrinos: status, models, string theory expectations Introduction Neutrino preliminaries and status Models String embeddings Intersecting brane The Z 3 heterotic orbifold Embedding the Higgs triplet Outlook
Particle Physics: Neutrinos part I
Particle Physics: Neutrinos part I José I. Crespo-Anadón Week 8: November 10, 2017 Columbia University Science Honors Program Course policies Attendance record counts Up to four absences Lateness or leaving
Two hot issues in neutrino physics
Bari Xmas Workshop /1/011 Two hot issues in neutrino physics Antonio Palazzo Excellence Cluster Universe - TUM 1 Outline! - Introduction - The evidence of! 13 >0 - Hints of new light sterile neutrinos
Status and prospects of neutrino oscillations
Status and prospects of neutrino oscillations S. Bilenky JINR(Dubna)TRIUMF June 10, 2017 The award of the 2015 Nobel Prize to T. Kajita and A. McDonald for the discovery of neutrino oscillations, which
Particle Physics: Neutrinos part II
Particle Physics: Neutrinos part II José I. Crespo-Anadón Week 9: November 18, 2017 Columbia University Science Honors Program 3 evidences for 3 neutrinos 2 3 neutrinos: 3 charged leptons Neutrinos are
Grand Unification Theories
Grand Unification Theories After the success of the unified theroy of electroweak interactions it was natural to ask if strong interactions are united with the weak and em ones. The greater strength of
Neutrino History ... and some lessons learned
2009 Neutrino Summer School Neutrino History accelerator, atmospheric, reactor and solar experiments... and some lessons learned Karsten M. Heeger University of Wisconsin History of Neutrino Physics -
arxiv: v1 [hep-ph] 6 Mar 2014
![arxiv: v1 [hep-ph] 6 Mar 2014](/thumbs/92/108507687.jpg "arxiv: v1 [hep-ph] 6 Mar 2014")
A predictive model of Dirac Neutrinos OSU-HEP-14-03 Shreyashi Chakdar, Kirtiman Ghosh and S. Nandi Department of Physics and Oklahoma Center for High Energy Physics, Oklahoma State University, Stillwater
Recent results from Super-Kamiokande
Recent results from Super-Kamiokande ~ atmospheric neutrino ~ Yoshinari Hayato ( Kamioka, ICRR, U-Tokyo ) for the Super-Kamiokande collaboration 1 41.4m Super-Kamiokande detector 50000 tons Ring imaging
Neutrino Physics: Lecture 1
Neutrino Physics: Lecture 1 Overview: discoveries, current status, future Amol Dighe Department of Theoretical Physics Tata Institute of Fundamental Research Feb 1, 2010 Plan of the course Omnipresent
Long & Very Long Baseline Neutrino Oscillation Studies at Intense Proton Sources. Jeff Nelson College of William & Mary
Long & Very Long Baseline Neutrino Oscillation Studies at Intense Proton Sources Jeff Nelson College of William & Mary Outline A highly selective neutrino primer Oscillations (what & why we believe) >
- Future Prospects in Oscillation Physics -
Measuring θ 13 and the Search for Leptonic CP Violation - Future Prospects in Oscillation Physics - Karsten M. Heeger Lawrence Berkeley National Laboratory ν e flux θ 13 =? P ee, (4 MeV) 1/r 2 Evidence
Finding an Upper Bound on Neutrinos Mass
Finding an Upper Bound on Neutrinos Mass Cindy Lin Department of Physics, Drexel University, Philadelphia, PA 19104 August 4, 2013 1 Introduction 1.1 Oscillation - Neutrinos have mass! The electron neutrino
Understanding the Particle Nature of Neutrinos
Understanding the Particle Nature of Neutrinos Karsten M. Heeger Lawrence Berkeley National Laboratory U e2 U µ2 * S = 2J U e3 U µ3 * U e1 U µ1 * Particle Properties Interactions Flavors & States Charge
Sterile neutrino oscillations
Sterile neutrino oscillations after first MiniBooNE results GDR Neutrino, APC Paris, 22 June 2007 Thomas Schwetz CERN T. Schwetz, GDR Neutrino, Paris, 22 June 2007 p.1 Outline Introduction to the LSND
Neutrinos: Yesterday, Today and Tomorrow. Stanley Wojcicki SLAC Summer Institute 2010 August 13, 2010
Neutrinos: Yesterday, Today and Tomorrow August 13, 2010 1 My Marching Orders 2 My Marching Orders...the summary talk should be visionary, rather than a dedicated summary of the SSI program. 2 My Marching
Today. Neutrinos Next: Neutrinos and the New Paradigm Neutrinos and the Unexpected Neutrinos and the Cosmos
The plan: Neutrinos Now... Today Neutrinos Next: Neutrinos and the New Paradigm Neutrinos and the Unexpected Neutrinos and the Cosmos Neutrino Opportunities Tomorrow Today Tomorrow Tomorrow 1 Neutrinos
NEUTRINO COSMOLOGY. ν e ν µ. ν τ STEEN HANNESTAD UNIVERSITY OF AARHUS PARIS, 27 OCTOBER 2006
NEUTRINO COSMOLOGY ν e ν µ ν τ STEEN HANNESTAD UNIVERSITY OF AARHUS PARIS, 27 OCTOBER 2006 OUTLINE A BRIEF REVIEW OF PRESENT COSMOLOGICAL DATA BOUNDS ON THE NEUTRINO MASS STERILE NEUTRINOS WHAT IS TO COME
Kinematic searches. Relativity. Uncertainty. Best candidate: Using molecular tritium, daughter will be Kai Zuber 25
Kinematic searches Relativity Uncertainty Best candidate: Using molecular tritium, daughter will be 12.06.2014 Kai Zuber 25 Tritium beta decay Half-life :12.3 years Matrix element: 5.55 Endpoint energy:
Long baseline experiments
Mauro Mezzetto, Istituto Nazionale Fisica Nucleare, Padova Long baseline experiments Present Status Concepts, strategies, challenges The two players: Dune and Hyper-Kamiokande Conclusions M. Mezzetto,
Neutrino Oscillation and CP violation
Neutrino Oscillation and CP violation Contents. Neutrino Oscillation Experiments and CPV. Possible CP measurements in TK 3. Summary Nov.4, 4 @Nikko K. Nishikawa Kyoto niversity CP Violation Asymmetry between
Fundamentals of Neutrino Physics and Astrophysics
Fundamentals of Neutrino Physics and Astrophysics Carlo Giunti Istituto Nazionale di Fisica Nucleare, Sezione di Torino and Dipartimento di Fisica Teorica, Universita di Torino, Italy Chung W. Kim Korea
MiniBooNE, LSND, and Future Very-Short Baseline Experiments
1 MiniBooNE, LSND, and Future Very-Short Baseline Experiments Mike Shaevitz - Columbia University BLV2011 - September, 2011 - Gatlinburg, Tennessee Neutrino Oscillation Summary 2! µ "! Sterile "! e New
Neutrinos, Oscillations and New Physics: An Introduction
Neutrinos, Oscillations and New Physics: An Introduction Rex Tayloe Indiana University, Dept. of Physics, Bloontington, Indiana, 47405 Abstract. An introduction to the neutrino and neutrino oscillations
Chart of Elementary Particles
Chart of Elementary Particles Chart of Elementary Particles Better Chart! Better Chart! As of today: Oscillation of 3 massive active neutrinos is clearly the dominant effect: If neutrinos have mass: For
Chapter 2 Neutrino Oscillation
Chapter Neutrino Oscillation Physics works, and I m still alive. Walter Lewin. Neutrinos and the Standard Model of Particle Physics The Standard Model (SM) of particle physics is the theory describing
Finding Neutrinos Mass Upper Bound
Finding Neutrinos Mass Upper Bound Cindy Lin Department of Physics, Drexel University, Philadelphia, PA 19104 June 7, 2013 1 Introduction 1.1 Oscillation - Neutrinos have mass! The electron neutrino is
arxiv:hep-ph/ v1 19 Jun 2004
Democratic Neutrino Mixing Reexamined Harald Fritzsch Sektion Physik, Universität München, Theresienstrasse 7A, 80 Munich, Germany arxiv:hep-ph/0400 v1 19 Jun 004 Zhi-zhong Xing Institute of High Energy
Analysis of Neutrino Oscillation experiments
Analysis of Neutrino Oscillation experiments Mario Andrés Acero Ortega Università degli Studi di Torino, LAPTH - Université de Savoie Second Year - Seminar Torino, Italy January 15th, 2008 Tutor: Carlo
Super-Kamiokande ~The Status of n Oscillation ~
May 26, 2006 Vulcano Workshop 2006 Super-Kamiokande ~The Status of n Oscillation ~ Yoshihisa OBAYASHI (ICRR, Univ. of Tokyo) for Super-Kamiokande Collaboration May 26, 2006 Y.Obayashi @ Vulcano 2006 1
Absolute Neutrino Mass from Cosmology. Manoj Kaplinghat UC Davis
Absolute Neutrino Mass from Cosmology Manoj Kaplinghat UC Davis Kinematic Constraints on Neutrino Mass Tritium decay (Mainz Collaboration, Bloom et al, Nucl. Phys. B91, 273, 2001) p and t decay Future
PLAN. Lecture I: Lecture II: Neutrino oscillations and the discovery of neutrino masses and mixings. Lecture III: The quest for leptonic CP violation
PLAN Lecture I: Neutrinos in the SM Neutrino masses and mixing: Majorana vs Dirac Lecture II: Neutrino oscillations and the discovery of neutrino masses and mixings Lecture III: The quest for leptonic
TeV-scale type-i+ii seesaw mechanism and its collider signatures at the LHC
TeV-scale type-i+ii seesaw mechanism and its collider signatures at the LHC Wei Chao (IHEP) Outline Brief overview of neutrino mass models. Introduction to a TeV-scale type-i+ii seesaw model. EW precision
Reactor Neutrino Oscillation Experiments: Status and Prospects
6! 5! 4! 1 2! 3!! Reactor Neutrino Oscillation Experiments: Status and Prospects Survival Probability 1 0.8 0.6 0.4 0.2 0 20 4! 15 Karsten M. Heeger University of Wisconsin Data - BG - Geo & e 99.73% C.L.
Overview of cosmological constraints on neutrino mass, number, and types
Overview of cosmological constraints on neutrino mass, number, and types Preliminaries Big Bang Nucleosynthesis Large Scale Structure and CMB Brief Comments Supernovae Magnetic Moments Decays Ultra High
m νe < 2.9 ev [26] (4) 2. Neutrinoless double β-decay and 3 H β-decay experiments
![m νe < 2.9 ev [26] (4) 2. Neutrinoless double β-decay and 3 H β-decay experiments](/thumbs/96/126546303.jpg "m νe < 2.9 ev [26] (4) 2. Neutrinoless double β-decay and 3 H β-decay experiments")
10 January 2002 Physics Letters B 524 (2002) 319 331 www.elsevier.com/locate/npe Searching for the CP-violation associated with Majorana neutrinos S. Pascoli a,b,s.t.petcov a,b,1,l.wolfenstein c a Scuola
Solar Neutrinos: Status and Prospects. Marianne Göger-Neff
Solar Neutrinos: Status and Prospects Marianne Göger-Neff NIC 2014, Debrecen TU München Solar Neutrinos Objective of the first solar neutrino experiment: to see into the interior of a star and thus verify
Solar spectrum. Nuclear burning in the sun produce Heat, Luminosity and Neutrinos. pp neutrinos < 0.4 MeV
SOLAR NEUTRINOS Solar spectrum Nuclear burning in the sun produce Heat, Luminosity and Neutrinos pp neutrinos < 0.4 MeV Beryllium neutrinos 0.86 MeV Monochromatic since 2 body decay 2 kev width due to
Updated three-neutrino oscillation parameters from global fits
Updated three-neutrino oscillation parameters from fits (Based on arxiv:14.74) Mariam Tórtola IFIC, Universitat de València/CSIC 37th International Conference on High Energy Physics 3th July 214, Valencia.
Search for sterile neutrino mixing in the muon neutrino to tau neutrino appearance channel with the OPERA detector
Search for sterile neutrino mixing in the muon neutrino to tau neutrino appearance channel with the OPERA detector INFN - Sezione di Bologna, I-4017 Bologna, Italy E-mail: matteo.tenti@bo.infn.it The OPERA
ν?? Solar & Atmospheric Oscillation Experiments Greg Sullivan University of Maryland Aspen Winter Conference January 21, 1999 )Past )Present )Future
Solar & Atmospheric Oscillation Experiments Greg Sullivan of Maryland Aspen Winter Conference January 21, 1999 ν?? e )Past z Neutrino Mass Mass & Oscillations )Present z Atmospheric neutrinos z Solar Solar
Latest Results from MINOS and MINOS+ Will Flanagan University of Texas on behalf of the MINOS+ Collaboration
Latest Results from MINOS and MINOS+ Will Flanagan University of Texas on behalf of the MINOS+ Collaboration Outline Overview of the Main Injector Neutrino Oscillation Search Detector Exciting physics
K. Zuber, TU Dresden DESY, 9/10 September In search of neutrinoless double beta decay
K. Zuber, TU Dresden DESY, 9/10 September 2008 In search of neutrinoless double beta decay Contents General Introduction Neutrino physics and DBD Experimental considerations GERDA COBRA SNO+ Outlook and
Probing Neutrino Properties with Astrophysics: Neutrino Masses
Probing Neutrino Properties with Astrophysics: Neutrino Masses Yong-Yeon Keum IBS/Seoul National University, Seoul Korea International Workshop on UNICOS 2014 13-15 May, 2014 Panjab University, Chandigarh,
New Results for ν µ ν e oscillations in MINOS
New Results for ν µ ν e oscillations in MINOS Jelena Ilic Rutherford Appleton Lab 4/28/10 RAL PPD Seminar 1 Neutrino Mixing Mass eigenstates flavour eigenstates Maki-Nakagawa-Sakata: Flavour composition
10 Neutrino Oscillations
10 Neutrino Oscillations 10.1 Neutrino mixing Particles are produced in interactions. The interaction process defines the properties of the emitted particle, for example it is a photon or an axion. Depending
Physics Potential of existing and future LBL ν beams
Mauro Mezzetto Istituto Nazionale di Fisica Nucleare, Sezione di Padova Physics Potential of existing and future LBL ν beams NBI 2002, March 14-18,2002, - CERN M. Mezzetto, Physics Potential of existing
The Oscillating Neutrino (experiments) Summary
The Oscillating Neutrino (experiments) Summary Introduction : Neutrino masses and oscillations Neutrino sources and experiments: reactors, accelerators, cosmic rays, sun Future Possible evidence for oscillations: