Phenomenology of Sterile Neutrinos Carlo Giunti
|
|
|
- Herbert Wells
- 7 years ago
- Views:
Transcription
1 Phenomenology of Sterile Neutrinos Carlo Giunti INFN, Sezione di Torino, and Dipartimento di Fisica Teorica, Università di Torino Neutrino Unbound: Neutrini in Cosmologia Scuola di Formazione Professionale INFN May 011, Padova C. Giunti Phenomenology of Sterile Neutrinos 16 May 011 1/59
2 Three-Neutrino Mixing Paradigm ¼ ½ Homestake Kamiokande GALLEX/GNO & SAGE Super-Kamiokande Solar e Reactor e disappearance Atmospheric Accelerator disappearance ¼ SNO BOREXino (KamLAND) Kamiokande IMB Super-Kamiokande MACRO Soudan- (KK & MINOS) ½ m SOL ³ ev sin SOL ³ 03 m ATM ³ ev sin ATM ³ 050 Two scales of m µ Three-Neutrino Mixing m SOL = m 1 ³ ev m ATM ³ m 31 ³ m 3 ³ ev C. Giunti Phenomenology of Sterile Neutrinos 16 May 011 /59
3 Three-Neutrino Mixing «L = 3 k=1 U «k kl («= e ) three flavor fields: e,, three massive fields: 1,, 3 m 1 + m 3 + m 13 = m m 1 +m 3 m +m 1 m 3 = 0 m SOL = m 1 ³ ev m ATM ³ m 31 ³ m 3 ³ ev C. Giunti Phenomenology of Sterile Neutrinos 16 May 011 3/59
4 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 Phenomenology of Sterile Neutrinos 16 May 011 4/59
5 LSND [LSND, PRL 75 (1995) 650; PRC 54 (1996) 685; PRL 77 (1996) 308; PRD 64 (001) 11007] e L ³ 30m 0MeV E 00MeV Beam Excess Beam Excess p(ν _ µ ν_ e,e+ )n p(ν _ e,e+ )n other L/E ν (meters/mev) m (ev /c 4 ) Karmen Bugey 90% (L max -L <.3) 99% (L max -L < 4.6) CCFR NOMAD sin θ m LSND 0eV ( m ATM m SOL) C. Giunti Phenomenology of Sterile Neutrinos 16 May 011 5/59
6 MiniBooNE Neutrinos [PRL 98 (007) 31801; PRL 10 (009) 10180] e L ³ 541m 475MeV E 3GeV Events / MeV Data ν e from µ + ν e from K 0 ν e from K π 0 misid Nγ dirt other Total Background QE E ν (GeV) Excess Events / MeV 0.8 data - expected background best-fit ν µ ν e 0.6 sin θ=0.004, m =1.0eV 0.4 sin θ=0., m =0.1eV QE E ν (GeV) [MiniBooNE, PRL 10 (009) 10180, arxiv:081.43] Low-Energy Anomaly! [Djurcic, arxiv: ] C. Giunti Phenomenology of Sterile Neutrinos 16 May 011 6/59
7 Events/MeV 0. MiniBooNE Antineutrinos [PRL 103 (009) ; PRL 105 (010) ] e L ³ 541m 475MeV E 3GeV 0.6 +/- ν e & ν e from µ Fit Region +/- ν e & ν e from K 0 ν e & ν e from K 0 π misid 0.4 Nγ dirt other Constr. Syst. Error Best Fit (E>475MeV) ) % CL 90% CL 99% CL KARMEN 90% CL BUGEY 90% CL /c Events/MeV Data - expected background Best Fit sin θ=0.004, m =1.0eV (ev m sin θ=0.03, m =0.3eV LSND 90% CL QE E ν (GeV) [MiniBooNE, PRL 105 (010) , arxiv: ] LSND 99% CL Agreement with LSND e signal! - 10 sin (θ) Similar LE but different L and E =µ Oscillations! C. Giunti Phenomenology of Sterile Neutrinos 16 May 011 7/59
8 Beyond Three-Neutrino Mixing ν τ ν s1 ν µ ν e ν ν 3 ν 4 ν 5 ν 1 m 1 m m 3 ν s m 4 m 5 logm m SOL 3ν-mixing m ATM m SBL C. Giunti Phenomenology of Sterile Neutrinos 16 May 011 8/59
9 Standard Model Neutrinos are the only massless fermions Neutrinos are the only fermions with only left-handed component L Extension of the SM: Massive Neutrinos Simplest extension: introduce right-handed component R Dirac mass m D R L + Majorana mass m M c R R el L L + er R R =µ 6 massive Majorana neutrinos C. Giunti Phenomenology of Sterile Neutrinos 16 May 011 9/59
10 Sterile Neutrinos Light anti- R are called sterile neutrinos c R s (left-handed) Sterile means no standard model interactions Active neutrinos ( e ) can oscillate into sterile neutrinos ( s ) Observables: Disappearance of active neutrinos Indirect evidence through combined fit of data (current indication) Powerful window on new physics beyond the Standard Model C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
11 Cross-section (pb) Number of Flavor and Massive Neutrinos? CESR DORIS PEP KEKB PEP-II PETRA TRISTAN Γ Z = Z SLC LEP I e + e hadrons =eγ Z + q=t W + W - LEP II Centre-of-mass energy (GeV) σ had [nb] [LEP, Phys. Rept. 47 (006) 57, arxiv:hep-ex/ ] Γ Zq q +Γ inv N = ALEPH DELPHI L3 OPAL average measurements, error bars increased by factor 10 ν 3ν 4ν E cm [GeV] Γ inv = N Γ Z C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
12 e + e Z invisible a a =µ e a=active 3 light active flavor neutrinos mixing µ «L = N k=1 U «k kl «= e Mass Basis: Flavor Basis: e s1 s ACTIVE STERILE N 3 no upper limit! C. Giunti Phenomenology of Sterile Neutrinos 16 May 011 1/59
13 Cosmology N s = number of thermalized sterile neutrinos (not necessarily integer) CMB and LSS in ΛCDM: [Hamann, Hannestad, Raffelt, Tamborra, Wong, PRL 105 (010) , arxiv: ] N s = m s 070eV (95% C.L.) [Giusarma, Corsi, Archidiacono, de Putter, Melchiorri, Mena, Pandolfi, arxiv: ] BBN: N s = [Cyburt, Fields, Olive, Skillman, AP 3 (005) 313, astro-ph/ ] N s = [Izotov, Thuan, ApJL 710 (010) L67, arxiv: ] C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
14 Direct Searches of Active-Sterile Transitions C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
15 CCFR [PRD 59 (1999) , arxiv:hep-ex/980903] NC interactions E 100GeV L ³ 14km C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
16 MINOS NC sample: 89% efficiency and 61% purity 97% of e -induced CC events misidentified as NC [arxiv: ] Events/GeV (GeV) E reco Near Detector Data Monte Carlo Prediction CC Background ν µ L ND = 104km Events/GeV (GeV) E reco L FD = 735km Far Detector Data θ 13 = 0 θ = 11.5, δ = π, m3 >0 13 ν µ CC Background -3 m 3 =.3 10 ev sin θ 3 = 1 Model 13 /D.O.F f s m 4 = m / / m 4 m / / C. Giunti Phenomenology of Sterile Neutrinos 16 May /59 90% C.L.
17 New Calculation of Reactor e Flux Th. A. Mueller, D. Lhuillier, M. Fallot, A. Letourneau, S. Cormon, M. Fechner, L. Giot, T. Lasserre, J. Martino, G. Mention, A. Porta, F. Yermia, Improved Predictions of Reactor Antineutrino Spectra, arxiv: detected flux normalization is increased by about 3% Emitted spectrum Cross-section Detected spectrum Arbitrary Units E ν (MeV) C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
18 G. Mention, M. Fechner, Th. Lasserre, Th. A. Mueller, D. Lhuillier, M. Cribier, A. Letourneau, The Reactor Antineutrino Anomaly, arxiv: ratio of observed and predicted event rates: deviation from unity at 98.4% C.L.: reactor antineutrino anomaly ILL Bugey 3/4 ROVNO Krasnoyarsk Goesgen Bugey3 Goesgen Krasnoyarsk 3 Goesgen Krasnoyarsk Bugey3 PaloVerde CHOOZ N OBS /(N EXP ) pred,new Distance to Reactor (m) C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
19 New reactor neutrino flux has several implications: fit of solar and KamLAND data, determination of 13, short-baseline e disappearance,... Chooz limit on 13 Hint of 13 0 [Chooz, EPJC 7 (003) 331] [Fogli et al., PRL 101 (008) ] dof χ contours CHOOZ simulation New spectra (σ f pred ) New spectra (σ f ano ) dof χ contours Old spectra New spectra (σ f pred ) New spectra (σ f ano ) CHOOZ (003) KamLAND (010) Solar (ev ) m sin θ sin (θ 13 ) tan θ 1 [Mention et al., arxiv: ] [Mention et al., arxiv: ] C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
20 Four-Neutrino Schemes: + and 3+1 m ν 4 m ν 4 ν 3 m SBL m SBL ν 3 ν ν + ν ν 1 C. Giunti Phenomenology of Sterile Neutrinos 16 May 011 0/59
21 + Four-Neutrino Schemes m m ν 4 ν m ATM ν 3 m SOL ν 1 m SBL m SBL ν m SOL ν 1 normal ν 4 m ATM ν 3 inverted C. Giunti Phenomenology of Sterile Neutrinos 16 May 011 1/59
22 + Schemes are strongly disfavored by solar and atmospheric data 50 χ solar + KamLAND solar solar (pre SNO salt) global solar + KamLAND χ PG χ PC 10 99% CL (1 dof) atm + KK + SBL η s η s matter effects + SNO NC 99% CL: s = U s1 + U s 1 s = U s3 + U s4 matter effects s 05 (solar + KamLAND) s 075 (atmospheric + KK) [Maltoni, Schwetz, Tortola, Valle, New J. Phys. 6 (004) 1, arxiv:hep-ph/040517] C. Giunti Phenomenology of Sterile Neutrinos 16 May 011 /59
23 3+1 Four-Neutrino Schemes m m m m ν ν 4 ν 4 ν 3 m SOL m ATM ν m ATM ν 1 m SOL ν 1 ν 3 m SBL m SBL m SBL m SBL ν 3 ν m SOL m ATM ν m ATM ν 1 m SOL ν 4 ν 4 ν 1 ν 3 normal 3-inverted 4-inverted fully-inverted Perturbation of 3- Mixing U e4 1 U 4 1 U 4 1 U s4 ³ 1 C. Giunti Phenomenology of Sterile Neutrinos 16 May 011 3/59
24 P «= = Effective SBL Oscillation Probabilities in 3+1 Schemes 4 k=1 4 k=1 U «ku ke ie kt U «ku ke i(e k E 1)t e ie 1t 4 k=1 U «ku k exp m k1 L E E k ³ p + m k m1 L m31 1 L p E E P «= U «1 U 1 +U «U +U «3 U 3 +U «4 m U L 4exp E 1 m 41 m U «1U 1 +U «U +U «3U 3 = Æ «U «4U 4 C. Giunti Phenomenology of Sterile Neutrinos 16 May 011 4/59
25 P «= Æ «U «4 U 4 = Æ «+ U «4 U 4 Æ «U «4 m L 1 exp E cos m L E 1 cos m L E = Æ «U «4 Æ «U 4 1 cos m L E = Æ «4U «4 Æ «U 4 sin m L E «= =µ P «= 4U «4 U 4 sin m L 4E «= =µ P ««= 4U «4 1 U «4 sin m L 4E C. Giunti Phenomenology of Sterile Neutrinos 16 May 011 5/59
26 m P «= sin «sin L 4E P ««m = 1 sin ««sin L 4E sin «= 4U «4 U 4 No CP Violation! sin ««= 4U «4 1 U «4 Perturbation of 3 Mixing U e4 1 U 4 1 U 4 1 U s4 ³ 1 U e1 U e U e3 U e4 sin ««1 U = U µ1 U τ1 U µ U τ U µ3 U τ3 U µ4 U τ4 U s1 U s U s3 U s4 SBL U «4 ³ sin ««4 C. Giunti Phenomenology of Sterile Neutrinos 16 May 011 6/59
27 10 10 m [ev ] Schemes GoF = 3% 10 1 PGoF = 089% % C.L. ν µ >ν e : LSND+KARMEN+MiniBooNE ν µ >ν e : MiniBooNE sin ϑ eµ Tension between LSND + KARMEN + MiniBooNE e and MiniBooNE e =µ CP Violation? 3+ =µ CP Violation OK [Sorel, Conrad, Shaevitz, PRD 70 (004) , hep-ph/030555; Maltoni, Schwetz, PRD 76, (007), arxiv: ; Karagiorgi et al, PRD 80 (009) , arxiv: ] 3+1+NSI =µ CP Violation OK [Akhmedov, Schwetz, JHEP 10 (010) 115, arxiv: ] C. Giunti Phenomenology of Sterile Neutrinos 16 May 011 7/59
28 e Disappearance and Disappearance 10 Reactor Rates 99.00% C.L. Bugey 3 (1995) Bugey 4 (1994) + Rovno (1991) Gosgen (1986) + ILL (1995) Krasnoyarsk (1994) % C.L. CDHSW (1984): ν µ ATM: ν µ + ν µ m [ev ] 1 m [ev ] sin ϑ ee New Reactor e Fluxes [Mueller et al., arxiv: ] [Mention et al., arxiv: ] sin ϑ µµ ATM constraint on U 4 [Maltoni, Schwetz, PRD 76 (007) , arxiv: ] C. Giunti Phenomenology of Sterile Neutrinos 16 May 011 8/59
29 e disappearance experiments: sin ee = 4U e4 1 U e4 ³ 4U e4 disappearance experiments: sin = 4U 4 1 U 4 ³ 4U 4 e experiments: sin e = 4U e4 U 4 ³ 1 4 sin ee sin Upper bounds on sin ee and sin =µ strong limit on sin e [Okada, Yasuda, Int. J. Mod. Phys. A1 (1997) , arxiv:hep-ph/ ] [Bilenky, Giunti, Grimus, Eur. Phys. J. C1 (1998) 47, arxiv:hep-ph/960737] C. Giunti Phenomenology of Sterile Neutrinos 16 May 011 9/59
30 3+1 Schemes % C.L. Reactors CDHSW + Atm Disappearance LSND + MBν 10 m [ev ] sin ϑ eµ C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
31 % C.L. MBν + LSNDν Dis + KARMEN + MBν 10 m [ev ] 1 PGoF = 0006% sin ϑ eµ Strong tension between e appearance and disappearance limits ( e e and mainly ) Tension reduced in 3+, 3+1+NSI CPT Violation? [Barger, Marfatia, Whisnant, PLB 576 (003) 303] [Giunti, Laveder, PRD 8 (010) , PRD 83 (011) ] C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
32 Antineutrino Oscillations in 3+1 Schemes m [ev ] 1 + m [ev ] ν (3+1) 10 1 ν (3+1) 68.7% C.L. (1σ) 90.00% C.L % C.L. (σ) 99.00% C.L % C.L. (3σ) 68.7% C.L. (1σ) 90.00% C.L % C.L. (σ) 99.00% C.L % C.L. (3σ) sin ϑ eµ sin ϑ µµ min = 870 NdF = 83 GoF = 36% m = 04eV sin e = 0016 sin ee = 000 sin = 065 Prediction: large SBL disappearance at m 01eV [Giunti, Laveder, PRD 83 (011) , arxiv: ] C. Giunti Phenomenology of Sterile Neutrinos 16 May 011 3/59
33 Gallium Anomaly Gallium Radioactive Source Experiments Tests of the solar neutrino detectors GALLEX (Cr1, Cr) and SAGE (Cr, Ar) Detection Process: e + 71 Ga 71 Ge+e e Sources: e + 51 Cr 51 V+ e e + 37 Ar 37 Cl+ e 51 Cr 37 Ar E [kev] B.R Ar (35.04 days) 37Cl (stable) 813 kev ν ( 9.8%) 811 kev ν (90.%) [SAGE, PRC 73 (006) , nucl-ex/051041] [SAGE, PRC 59 (1999) 46, hep-ph/ ] C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
34 1.1 GALLEX Cr1 SAGE Cr p(measured)/p(predicted) GALLEX Cr SAGE Ar [SAGE, PRC 73 (006) , nucl-ex/051041] R Gallex-Cr1 B = RB Gallex-Cr = RB SAGE-Cr = RB SAGE-Ar = [SAGE, PRC 59 (1999) 46, hep-ph/ ] L GALLEX = 19m L SAGE = 06m R Ga B = Bahcall cross section Only exp uncertainties! C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
35 Deficit could be due to overestimate of ( e + 71 Ga 71 Ge+e ) Calculation: Bahcall, PRC 56 (1997) 3391, hep-ph/ / MeV 3/ 71 Ga 5/ MeV 1/ 71 Ge 0.33 MeV G.S. related to measured (e + 71 Ge 71 Ga+ e ): ( 51 Cr) = G.S. ( 51 Cr) G.S. ( 51 Cr) = cm (1 0004) 3 Contribution of Excited States only 5%! BGT 175keV +00 BGT 500keV BGT G.S. BGT G.S. C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
36 Bahcall: [Bahcall, PRC 56 (1997) 3391, hep-ph/ ] from p + 71 Ga 71 Ge+n measurements [Krofcheck et al., PRL 55 (1985) 1051] BGT 175keV 0056 µ BGT 175keV = 0056 BGT G.S. BGT G.S. 3 lower limit: BGT 175keV BGT G.S. = BGT 500keV BGT G.S. = 0 3 upper limit: BGT 175keV BGT G.S ( 51 Cr) = cm Haxton: 1 BGT 500keV BGT G.S. = 0146 BGT 500keV BGT G.S. = 0146 =µ R Ga B = [Hata, Haxton, PLB 353 (1995) 4, nucl-th/ ; Haxton, PLB 431 (1998) 110, nucl-th/ ] a sophisticated shell model calculation is performed... for the transition to the first excited state in 71 Ge. The calculation predicts destructive interference between the (pn) spin and spin-tensor matrix elements. ( 51 Cr) = cm (1 0106) 1 =µ R Ga H = C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
37 RH Ga = R Ga = R Ga exp RGa the exp and the uncertainties added in quadrature probability distribution of ratio is not Gaussian p(r) p R Ga Gallium B GALLEX Cr1 GALLEX Cr SAGE Cr SAGE Ar p R Ga p R Ga(r) = ½ p R Ga R Ga gs (rs)p exp R Ga (s)s ds R Ga = the R Gallex-Cr1 = R Gallex-Cr = R SAGE-Cr = R SAGE-Ar = [Giunti, Laveder, arxiv: ] r C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
38 Gallium Radioactive Source Experiments are Short-BaseLine Neutrino Oscillation Experiments [Bahcall, Krastev, Lisi, PLB 348 (1995) 11] C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
39 m P SBL (LE) = 1 ee sin sin L 4E Êk È R k (sin m ) = dv L i bk i i k P SBL (LE ee i) Êk dv L È i bk i k i k = GALLEX-Cr1 GALLEX-Cr SAGE-Cr SAGE-Ar R k = R k exp Rk the p R (r) = ½ R k gs fully correlated theoretical uncertainty! k p R k exp (r k s) p R k the (s)s 4 ds Ä(sin m ) = p R ( R(sin m )) (sin m ) = ln Ä(sin m )+constant C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
40 χ Gallium 68.7% C.L. (1σ) 90.00% C.L % C.L. (σ) 99.00% C.L % C.L. (3σ) No Osc. = 97 No Osc. disfavored at 99.3 % C.L (7) m [ev ] 1 + Osc. sin bf = 051 m bf = 4eV sin ϑ χ [Giunti, Laveder, arxiv: ] C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
41 Reactor Antineutrino Anomaly R Reactor Rates Bugey3 15 Bugey3 40 Bugey3 95 Bugey4 ROVNO Gosgen 38 Gosgen 45 Gosgen 65 ILL Krasno 33 Krasno 9 Krasno L [m] Best Fits Reactor Rates Bugey 3 Spectra Combined R R R New Reactor Neutrino Flux Bugey 3 Spectra L = 15 m E e + [MeV] New Reactor Neutrino Flux Bugey 3 Spectra L = 40 m E e + [MeV] New Reactor Neutrino Flux Bugey 3 Spectra L = 95 m R rates = Improved hint of oscillations given by Bugey energy spectrum with old reactor fluxes sin bf = 0059 mbf = 189eV E e + [MeV] [Acero, Giunti, Laveder, PRD 78 (008) , arxiv:0711.4] C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
42 Reactor Antineutrino Anomaly Gallium Neutrino Anomaly m [ev ] 1 m [ev ] 1 Reactors Gallium 68.7% C.L. (1σ) 90.00% C.L % C.L. (σ) 99.00% C.L % C.L. (3σ) 68.7% C.L. (1σ) 90.00% C.L % C.L. (σ) 99.00% C.L % C.L. (3σ) sin ϑ sin ϑ sin bf = 0059 sin bf = 051 m bf = 189eV m bf = 4eV C. Giunti Phenomenology of Sterile Neutrinos 16 May 011 4/59
43 Gallium Anomaly + Reactor Anomaly min = 596 NdF = 71 m [ev ] 1 GoF = 83% sin = 011 m = 95eV 95.00% C.L. Gallium Reactors Combined PGoF = 46% sin ϑ C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
44 Old Reactor e Fluxes New Reactor e Fluxes χ % 99% 95.45% 90% 68.7% Gallium Reactors Gallium + Reactors χ % 99% 95.45% 90% 68.7% Gallium Reactors Gallium + Reactors sin ϑ PGoF = 3% sin ϑ PGoF = 46% C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
45 3 H 3 He+e + e K(T) = ÚÙ Ù Ø 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 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 Phenomenology of Sterile Neutrinos 16 May /59
46 Neutrino Mixing =µ K(T) = (Q T) k U ek Õ(Q T) m k 1 Ã Ì µ ¼º¾ Í ¾ ½ ¼ ѽ ½¼ Î ¼º½ Í ¾ ¾ ¼ Ѿ ½¼¼ Î ¼º½ ¼º¼ ¼ ½º ½º ½º ½º ½º É Ñ ¾ Ì É Ñ ½ analysis of data is different from the no-mixing case: N 1 parameters k U ek = 1 if experiment is not sensitive to masses (m k Q T) effective mass: m = k U ek m k K = (Q T) U ek m 1 k ³ (Q T) (Q T) U ek 1 1 mk (Q T) k k Õ = (Q T) 1 1 m ³ (Q T) (Q T) m (Q T) C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
47 Neutrinoless Double-Beta Decay + β As 0 + β 76 3Ge β β 0 + Effective Majorana Neutrino Mass: m = k 76 34Se U ek m k C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
48 Two-Neutrino Double- Decay: L = 0 Æ(AZ) Æ(AZ +)+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 Phenomenology of Sterile Neutrinos 16 May /59
49 Implications of Gallium and Reactor Anomalies Decay ( ) 0 Decay χ % Gallium Reactors Tritium Combined 99% 95.45% 90% 68.7% U e4 m [ev] χ m = U ek mk m = k [Giunti, Laveder, In Preparation] 99.73% Gallium Reactors Tritium Combined 99% 95.45% 90% 68.7% U e4 m [ev] U ek m k k C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
50 MiniBooNE Low-Energy Anomaly Events / MeV Data ν e from µ + ν e from K 0 ν e from K π 0 misid Nγ dirt other Total Background [PRL 10 (009) 10180, arxiv:081.43] Our Hypothesis: Nj the = f P een cal e j +N cal j QE E ν [Giunti, Laveder, PRD 77 (008) 09300, arxiv: ; PRD 80 (009) , arxiv: ] C. Giunti Phenomenology of Sterile Neutrinos 16 May /59 (GeV)
51 Nj the = f P een cal e j +N cal j Estimated 15% uncertainty of the calculated neutrino flux [MiniBooNE, PRD 79 (009) 0700, arxiv: ] is consistent with measured ratio of detected and predicted charged-current quasi-elastic events [MiniBooNE, PRL 100 (008) 03301, arxiv: ] We fit MiniBooNE e and data using the info at C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
52 events / MeV E [MeV] MiniBooNE ν e N νe,the (j) νe,cal νe,j = f ν P νe νe N νe,j νµ,the νµ,cal N νe,j = f ν N νe,j N the νe,j = N νe,the νµ,the νe,j + N νe,j (b) [Giunti, Laveder, PRD 8 (010) , arxiv: ] No Osc. & f = 1 min = NdF = 3+16 GoF = 41% Our Hypothesis min = 0+76 NdF = 16 GoF = 89% f = 16 sin = 03 m = 184eV C. Giunti Phenomenology of Sterile Neutrinos 16 May 011 5/59
53 MiniBooNE + Gallium m [ev ] χ MB + Ga 68.7% C.L. (1σ) 95.45% C.L. (σ) 99.73% C.L. (3σ) min = 3+9 NdF = 0 GoF = 93% sin = 07 m = 19eV PGoF = 93% sin ϑ χ [Giunti, Laveder, PRD 8 (010) , arxiv: ] C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
54 MiniBooNE + Gallium + Reactors χ dof χ contours 1 dof χ profile % % % (ev ) m new dof χ profile sin (θ new ) 5 10 χ [Mention et al., arxiv: ] C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
55 Future MiniBooNE is continuing to take antineutrino data. e + ICARUS@CERN-PS: L 1km E 1GeV [C. Rubbia et al, CERN-SPSC ] ( ) ( ) e + ( ) ( ) + ( ) e ( ) e MicroBooNE will test the MiniBooNE low-energy anomaly by measuring 0 background. C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
56 e disappearance: new SAGE Gallium source experiments with spherical shells [Gavrin et al, arxiv: ] CPT test: e and e disappearance Beta-Beam experiments: [Antusch, Fernandez-Martinez, PLB 665 (008) 190, arxiv: ] N(AZ) N(AZ +1)+e + e ( ) N(AZ) N(AZ 1)+e + + e ( + ) Neutrino Factory experiments: [Giunti, Laveder, Winter, PRD 80 (009) , arxiv: ] + +e + + e +e + e C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
57 New e and e radioactive source experiments with low-threshold neutrino elastic scattering detectors. Borexino: ( ) e +e ( ) e +e [Pallavicini, talk at BEYOND3NU] [Ianni, Montanino, Scioscia, EPJC 8 (1999) 609, arxiv:hep-ex/990101] LENS (Low Energy Neutrino Spectroscopy): e In 115 Sn+e + e +p n+e + [Agarwalla, Raghavan, arxiv: ] E th = 01MeV E th = 18MeV Spherical Gaseous TPC: [Vergados, Giomataris, Novikov, arxiv: ] Targets: 131 Xe, 40 Ar, 0 Ne, 4 He. Sources: 37 Ar, 51 Cr, 65 Zn, 3 P. C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
58 Conclusions 1 Suggestive LSND and MiniBooNE agreement on SBL e Hint in favor of sterile neutrinos is compatible with cosmological data, but mass is limited Two experimental tensions: LSND and MiniBooNE e vs MiniBooNE e (CP violation?) LSND and MiniBooNE e vs e and disappearance limits CPT-invariant 3+1 Four-Neutrino Mixing is strongly disfavored (no CP violation and tension between appearance and disappearance) 3+ can explain CP violation and reduce tension between appearance and disappearance with New Reactor e Fluxes 3+1+NSI has CP violation and reduced appearance-disappearance tension CPT-violating 3+1 Mixing =µ testable large SBL disappearance C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
59 Conclusions Interesting possible agreement of Gallium Anomaly (SBL e disappearance) Reactor Anomaly (SBL e disappearance) Testable Predictions: m eV () m eV () Exciting experimental results in favor of sterile neutrinos. More work to do because interpretation is not clear: Explanation of all data needs at least two new physical effects. Without CPT violation tensions do not disappear completely. Possible that some experiments are giving misleading information. New short-baseline neutrino oscillation experiments are needed! C. Giunti Phenomenology of Sterile Neutrinos 16 May /59
Light sterile neutrinos in the early universe. Cecilia Lunardini Arizona State University
Light sterile neutrinos in the early universe Cecilia Lunardini Arizona State University ν s and cosmic radiation energy density Motivations and status how much room for ν s in the universe? Contribution
A global analysis of neutrino masses, mixings and phases: entering the new era of leptonic CP violation searches
XCVIII Congresso Nazionale Napoli 17-21 Settembre 2012 A global analysis of neutrino masses, mixings and phases: entering the new era of leptonic CP violation searches Gian Luigi Fogli Dipartimento di
Borexino and Neutrino Image Radiation Sources
Short Distance Neutrino Oscillations with BoreXino Heidelberg Jul. 10 th, 2013 Marco Pallavicini on behalf of the Borexino Collaboration Dipartimento di Fisica - Università di Genova & INFN Sezione di
CeSOX sensitivity studies
CeSOX sensitivity studies Ma#hieu VIVIER, Guillaume MENTION CEA- Saclay, DSM/IRFU/SPP CeSOX kick- off meecng Paris, February 5 th CeSOX experimental parameters L/E spectrum modeling and χ 2 Model computes
Flavor Ratios of Extragalactical Neutrinos and Neutrino Shortcuts in Extra Dimensions [arxiv:1410.0408]
![Flavor Ratios of Extragalactical Neutrinos and Neutrino Shortcuts in Extra Dimensions [arxiv:1410.0408]](/thumbs/34/17127788.jpg "Flavor Ratios of Extragalactical Neutrinos and Neutrino Shortcuts in Extra Dimensions [arxiv:1410.0408]")
Flavor Ratios of Extragalactical Neutrinos and Neutrino Shortcuts in Extra Dimensions [arxiv:1410.0408] E. Aeikens, H. Päs, S. Pakvasa, Philipp Sicking Content 1 Introduction 2 Model 3 Adiabatic Limit
Measurement of the pep and CNO solar neutrino interaction rates in Borexino
/tr Università degli studi di Genova Facoltà di scienze Matematiche, Fisiche e Naturali Scuola di Dottorato in Scienze e Tecnologie per l informazione e la conoscenza XXIV Ciclo, A.A. 2009-2012 A Thesis
The Solar Neutrino Problem
The Solar Neutrino Problem Martin Lahrz martin.lahrz@gmail.com University Umeå Abstract Since neutrinos are the only known particles being able to leave the core of the Sun directly, they were supposed
Single Electron Detection with the Large Volume Spherical Proportional Counter Ilias Savvidis
Single Electron Detection with the Large Volume Spherical Proportional Counter Ilias Savvidis Collaboration S. Andriamonje, S. Aune, E. Bougamont, M. Chapelier, P. Colas, J. Derré, E. Ferrer, G. Gerbier,
PROSPECT: Precision Reactor Oscillation and Spectrum experiment
PROSPECT: Precision Reactor Oscillation and Spectrum experiment DAVID MARTINEZ CAICEDO on behalf of PROSPECT collaboration ILLINOIS INSTITUTE OF TECHNOLOGY NUFACT 2015 AUGUST 14th 2015 1 Outline Motivations:
Search for double beta decay to excited states with CUORICINO and data acquisition system for CUORE
Università degli studi di Genova Facoltà di scienze Matematiche, Fisiche e Naturali Scuola di Dottorato in Scienze e Tecnologie per l informazione e la conoscenza XXI Ciclo, A.A. 2006-2009 A Thesis submitted
Ay 122 - Fall 2004. The Sun. And The Birth of Neutrino Astronomy. This printout: Many pictures missing, in order to keep the file size reasonable
Ay 122 - Fall 2004 The Sun And The Birth of Neutrino Astronomy This printout: Many pictures missing, in order to keep the file size reasonable Why Study the Sun? The nearest star - can study it in a greater
Standard and non-standard neutrino properties
1 Standard and non-standard neutrino properties J. W. F. Valle a a Instituto de Física Corpuscular C.S.I.C./Universitat de València Edificio Institutos de Paterna, Apt 2285, E 4671 València, Spain I review
T2K and Aggressive Oscillation
Can the hint of δ CP from T2K also indicate the hierarchy and octant? Monojit Ghosh Physical Research Laboratory Ahmedabad XXI DAE-BRNS High Energy Physics Symposium IITG, 8-12 December, 214 Introduction
ABOUT THE POSSIBILITY TO MEASURE SOME STANDARD MODEL PARAMETERS AND SEARCH FOR NEW PHYSICS WITH LOW ENERGY NEUTRINOS *
Romanian Reports in Physics, Vol. 64, No. 1, P. 4 3, 01 ELEMENTARY PARTICLE PHYSICS ABOUT THE POSSIBILITY TO MEASURE SOME STANDARD MODEL PARAMETERS AND SEARCH FOR NEW PHYSICS WITH LOW ENERGY NEUTRINOS
Selected Topics in Elementary Particle Physics ( Haupt-Seminar )
Selected Topics in Elementary Particle Physics ( Haupt-Seminar ) Paola Avella, Veronika Chobanova, Luigi Li Gioi, Christian Kiesling, Hans-Günther Moser, Martin Ritter, Pit Vanhoefer Time: Do, 12 ct -14
BOSTON UNIVERSITY GRADUATE SCHOOL OF ARTS AND SCIENCES. Dissertation PRECISE STUDY OF THE ATMOSPHERIC NEUTRINO
BOSTON UNIVERSITY GRADUATE SCHOOL OF ARTS AND SCIENCES Dissertation PRECISE STUDY OF THE ATMOSPHERIC NEUTRINO OSCILLATION PATTERN USING SUPER-KAMIOKANDE I AND II by FANNY MAUDE DUFOUR B.S., Université
Solar Neutrinos. Neutrino light from the Sun (Super-Kamiokande) energy of the neutrinos in MeV
Solar Neutrinos 4 p He 4 + 2e + + 2 ν e + 26.7 MeV Neutrino light from the Sun (Super-Kamiokande) energy of the neutrinos in MeV Solar Neutrinos: pioneering experiment Nobelprize 2002 Since 1970 ν e 37
Study of the B D* ℓ ν with the Partial Reconstruction Technique
Study of the B D* ℓ ν with the Partial Reconstruction Technique + University of Ferrara / INFN Ferrara Dottorato di Ricerca in Fisica Ciclo XVII Mirco Andreotti 4 March 25 Measurement of B(B D*ℓν) from
From beta- decay to neutrino- less double beta decay: The quest for Majorana neutrinos
From beta- decay to neutrino- less double beta decay: EPS Historic Site: The Neutrino Experiment at Debrecen by J. Csikai and A. Szalay Debrecen, Hungary October 25, 2013 Stefan Schönert Physik-Department,
arxiv:hep-ex/0502033v1 17 Feb 2005
arxiv:hep-ex/0502033v1 17 Feb 2005 NOSTOS experiment and new trends in rare event detection I.Giomataris a,s. Aune a, P. Colas a, E. Ferrer a, I. Irastorza a, B. Peyaud a, J. Dolbeau b, P. Gorodetzky b,
Discovery of neutrino oscillations
INSTITUTE OF PHYSICS PUBLISHING Rep. Prog. Phys. 69 (2006) 1607 1635 REPORTS ON PROGRESS IN PHYSICS doi:10.1088/0034-4885/69/6/r01 Discovery of neutrino oscillations Takaaki Kajita Research Center for
Solar neutrinos: from their production to their detection
: from their production to their detection Universitï degli Studi di Milano and Istituto Nazionale di Fisica Nucleare E-mail: Lino.Miramonti@mi.infn.it Nuclear fusion reactions take place in the core of
How To Find The Higgs Boson
Dezső Horváth: Search for Higgs bosons Balaton Summer School, Balatongyörök, 07.07.2009 p. 1/25 Search for Higgs bosons Balaton Summer School, Balatongyörök, 07.07.2009 Dezső Horváth MTA KFKI Research
Università degli studi di Bologna. Algorithms for the analysis of neutrino interactions in the OPERA-like Emulsion Cloud Chambers
Università degli studi di Bologna Facoltà di Scienze Matematiche Fisiche e Naturali Dottorato di Ricerca in Fisica XIX ciclo Algorithms for the analysis of neutrino interactions in the OPERA-like Emulsion
How NOT to do a data analysis
How NOT to do a data analysis The Physics case: neutrinoless double beta decay The experimental apparatus The reported results A critical review of the analysis The ROOT code A. Fontana and P. Pedroni
Status Report of the Gerda Phase II Startup
Status Report of the Gerda Phase II Startup Valerio D Andrea on behalf of the Gerda Collaboration Gran Sasso Science Institute (INFN), L Aquila ICNPA 2016 18th International Conference on Neutrino Physics
arxiv:hep-ph/0011247v2 5 Jan 2001
FERMILAB-Pub-00/300-T VAND TH 00 8 hep-ph/0011247 November 20, 2000 arxiv:hep-ph/0011247v2 5 Jan 2001 Optimizing T-violating Effects for Neutrino Oscillations in Matter Stephen J. Parke 1 and Thomas J.
WIMP dark matter and the isotropic radio signal Roberto A. Lineros R. Instituto de Física Corpuscular - CSIC/U. Valencia @Roberto_Lineros Outline Introduction Cosmic ray propagation Synchrotron emission
FRONTIERS OF LOW ENERGY NEUTRINO PHYSICS AND ASTROPHYSICS
FRONTIERS OF LOW ENERGY NEUTRINO PHYSICS AND ASTROPHYSICS Gioacchino Ranucci - I.N.F.N. Milano TAUP 0 ROME - 5 July, 200 1-Solar neutrinos and the SSM 2-Geo-neutrino detection, status and perspectives
Icarus and Status of Liquid Argon Technology
IL NUOVO CIMENTO Vol.?, N.?? Icarus and Status of Liquid Argon Technology A. Fava( 1 ), for the ICARUS Collaboration ( 1 ) I.N.F.N. - Sezione di Padova, Via Marzolo 8, I-35131 Summary. ICARUS-T600 at the
arxiv:hep-ph/0310009v1 1 Oct 2003
arxiv:hep-ph/319v1 1 Oct 23 HADRONISATION AT LEP ELI BEN-HAIM Laboratoire de l Accélérateur Linéaire (L.A.L.), Université Paris-Sud, Bâtiment 2, BP 34, F-91898 Orsay cedex, France An overview of recent
INTRODUCTION TO NEUTRINO PHYSICS
INTRODUCTION TO NEUTRINO PHYSICS Paolo Lipari Dipartimento di Fisica, Università di Roma la Sapienza, and I.N.F.N., Sezione di Roma, P.A. Moro, I-00185 Roma, Italy 1. INTRODUCTION Abstract Neutrino Physics
The origin of neutrino mass
New experimental data, which show that neutrinos have mass, are forcing theorists to revise the Standard Model of particle physics The origin of neutrino mass IF WE look deep into the universe, we see
arxiv:hep-ex/0106089 v1 25 Jun 2001
International Journal of Modern Physics A, c World Scientific Publishing Company OUNP-2001-03 AN EXPERIMENTALIST S VIEW OF NEUTRINO OSCILLATIONS arxiv:hep-ex/0106089 v1 25 Jun 2001 ANTONELLA DE SANTO Sub-Department
Nuclear Physics. Nuclear Physics comprises the study of:
Nuclear Physics Nuclear Physics comprises the study of: The general properties of nuclei The particles contained in the nucleus The interaction between these particles Radioactivity and nuclear reactions
Validation of the neutrino oscillation model and first real observation of geoneutrinos with Borexino
Validation of the neutrino oscillation model and first real observation of geoneutrinos with Borexino on behalf of the Borexino Collaboration SIF 2010 - Bologna 1-Solar neutrinos and the SSM 2-Performances
Highlights of Recent CMS Results. Dmytro Kovalskyi (UCSB)
Highlights of Recent CMS Results Dmytro Kovalskyi (UCSB) Introduction Number of CMS publication is over 0 already It is very hard to review all the recent results in one talk This talk concentrates on
The Mainz LXe TPC MC simulations for a Compton scattering experiment
The Mainz LXe TPC MC simulations for a Compton scattering experiment Pierre Sissol Johannes Gutenberg Universität Mainz 12 November 2012 1 / 24 Outline 1 Dark Matter 2 Principle of a dual-phase LXe TPC
Interstellar Cosmic-Ray Spectrum from Gamma Rays and Synchrotron
Interstellar Cosmic-Ray Spectrum from Gamma Rays and Synchrotron Chuck Naval Research Laboratory, Washington, DC charles.dermer@nrl.navy.mil Andy Strong Max-Planck-Institut für extraterrestrische Physik,
Theory versus Experiment. Prof. Jorgen D Hondt Vrije Universiteit Brussel jodhondt@vub.ac.be
Theory versus Experiment Prof. Jorgen D Hondt Vrije Universiteit Brussel jodhondt@vub.ac.be Theory versus Experiment Pag. 2 Dangerous cocktail!!! Pag. 3 The basics in these lectures Part1 : Theory meets
The Sudbury Neutrino Observatory has solved a 30-year-old mystery by showing that neutrinos from the sun change species en route to the earth
Solving the The Sudbury Neutrino Observatory has solved a 30-year-old mystery by showing that neutrinos from the sun change species en route to the earth By Arthur B. McDonald, Joshua R. Klein and David
arxiv:hep-ph/9607427v1 25 Jul 1996
DFTT 44/96 IFT-96-16 MPI-PhT/96-63 hep-ph/967427 arxiv:hep-ph/967427v1 25 Jul 1996 New proton polarized structure functions in charged current processes at HERA M. Anselmino, P. Gambino, J. Kalinowski,1
Identifying the Theory of Dark Matter with Direct Detection
Identifying the Theory of Dark Matter with Direct Detection Sam McDermott arxiv:1506.04454 and ascl.net/1506.002 with Vera Gluscevic, Moira Gresham, Annika H. G. Peter, and Kathryn Zurek Motivation Dark
Cross section, Flux, Luminosity, Scattering Rates
Cross section, Flux, Luminosity, Scattering Rates Table of Contents Paul Avery (Andrey Korytov) Sep. 9, 013 1 Introduction... 1 Cross section, flux and scattering... 1 3 Scattering length λ and λ ρ...
Standard Model of Particle Physics
Standard Model of Particle Physics Chris Sachrajda School of Physics and Astronomy University of Southampton Southampton SO17 1BJ UK SUSSP61, St Andrews August 8th 3rd 006 Contents 1. Spontaneous Symmetry
A SUSY SO(10) GUT with 2 Intermediate Scales
A SUSY SO(10) GUT with 2 Intermediate Scales Manuel Drees Bonn University & Bethe Center for Theoretical Physics SUSY SO(10) p. 1/25 Contents 1 Motivation: SO(10), intermediate scales SUSY SO(10) p. 2/25
Effect of energy scale imperfections on results of neutrino mass measurements from β-decay
Effect of energy scale imperfections on results of neutrino mass measurements from β-decay J. Kašpar 1, M. Ryšavý, A. Špalek and O. Dragoun Nuclear Physics Institute, Acad. Sci. Czech Rep., CZ 250 68 Řež
B I N G O B I N G O. Hf Cd Na Nb Lr. I Fl Fr Mo Si. Ho Bi Ce Eu Ac. Md Co P Pa Tc. Uut Rh K N. Sb At Md H. Bh Cm H Bi Es. Mo Uus Lu P F.
Hf Cd Na Nb Lr Ho Bi Ce u Ac I Fl Fr Mo i Md Co P Pa Tc Uut Rh K N Dy Cl N Am b At Md H Y Bh Cm H Bi s Mo Uus Lu P F Cu Ar Ag Mg K Thomas Jefferson National Accelerator Facility - Office of cience ducation
Curriculum Vitae of Carla Biggio
Curriculum Vitae of Carla Biggio last update: 13/10/2013 Personal Data Name Carla Biggio Place and Date of Birth Genova (Italy), 24/01/1976 Nationality Italian Present Address Dipartimento di Fisica, Università
Search for supersymmetric Dark Matter with GLAST!!
Search for supersymmetric Dark Matter with GLAST!! Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata ICCRC2003 The 28th International Cosmic Ray Conference Tsukuba, Japan, July 31-
Nuclear Displication of a Neutrini Ai Reattori - IFAE 2007
Oscillazioni di neutrini ai reattori Alessandra Tonazzo - Paris7 & APC Neutrini da reattori e misura di oscillazioni Un cenno a Δm 2 12 e KamLAND Misura di θ 13 Double Chooz Daya Bay, RENO, Angra. Un idea
Risultati recenti dell'esperimento CMS ad LHC e prospettive per il run a 14 TeV
Risultati recenti dell'esperimento CMS ad LHC e prospettive per il run a 14 TeV Luca Lista INFN Napoli 1 78 reconstructed vertices CMS experiment CMS recorded 5fb-1 at 7 TeV and 20 fb-1 at 8 TeV 2 Electroweak
Physik des Higgs Bosons. Higgs decays V( ) Re( ) Im( ) Figures and calculations from A. Djouadi, Phys.Rept. 457 (2008) 1-216
: Higgs decays V( ) Re( ) Im( ) Figures and calculations from A. Djouadi, Phys.Rept. 457 (2008) 1-216 1 Reminder 10.6.2014 Higgs couplings: 2 Reminder 10.6.2014 Higgs BF as a function of mh Higgs total
Radiative corrections to anti-neutrino proton scattering
Radiative corrections to anti-neutrino proton scattering Udit Raha, a b and Kuniharu Kubodera b a Indian Institute of Technology Guwahati, 78 039 Assam, India b Dept. Physics and Astronomy, University
arxiv:hep-lat/9704002v1 6 Apr 1997
Quenched Hadron Spectrum and Decay Constants on the Lattice L. Giusti 1 Scuola Normale Superiore, P.zza dei Cavalieri 7 and INFN, Sezione di Pisa, 56100 Pisa, Italy. Abstract arxiv:hep-lat/9704002v1 6
Letter of Intent Neutrino Oscillation Experiment at JHF
Letter of Intent Neutrino Oscillation Experiment at JHF Summary The first stage of a next-generation long baseline neutrino oscillation experiment is proposed to explore the physics beyond the Standard
REPORTS ON PROGRESS IN PHYSICS Rep. Prog. Phys. 64 (2001) 97 146 www.iop.org/journals/rp PII: S0034-4885(01)04040-4
INSTITUTE OF PHYSICS PUBLISHING REPORTS ON PROGRESS IN PHYSICS Rep. Prog. Phys. 64 (2001) 97 146 www.iop.org/journals/rp PII: S0034-4885(01)04040-4 Solar neutrinos Michael F Altmann 1,3, Rudolf L Mößbauer
HIGH-ENERGY COLLIDER PARAMETERS: e + e Colliders (I)
28. High-energy collider parameters 1 HIGH-ENERGY COLLIDER PARAMETERS: e + e Colliders (I) Updated in early 2012 with numbers received from representatives of the colliders (contact J. Beringer, LBNL).
Low- and high-energy neutrinos from gamma-ray bursts
Low- and high-energy neutrinos from gamma-ray bursts Hylke B.J. Koers Low- and high-energy neutrinos from gamma-ray bursts Hylke B.J. Koers HK and Ralph Wijers, MNRAS 364 (2005), 934 (astro-ph/0505533)
Reconstruction of neutrino. induced neutral current neutral. pion events with the T2K ND280. Tracker and ECAL
Imperial College London Department of Physics Reconstruction of neutrino induced neutral current neutral pion events with the T2K ND28 Tracker and ECAL Pawel Guzowski September 211 Submitted in part fulfilment
Search for Dark Matter at the LHC
Search for Dark Matter at the LHC Steven Lowette Vrije Universiteit Brussel - IIHE 19 November 2014 3rd CosPa Meeting Université de Liège Content Introduction Generic DM searches at the LHC Explicit DM
1 Introduction. 1 There may, of course, in principle, exist other universes, but they are not accessible to our
1 1 Introduction Cosmology is the study of the universe as a whole, its structure, its origin, and its evolution. Cosmology is soundly based on observations, mostly astronomical, and laws of physics. These
Single-Top Production at the Tevatron and the LHC: Results and Prospects
Single-Top Production at the Tevatron and the LHC: Results and Prospects Wolfgang Wagner Bergische Universität Wuppertal DESY Zeuthen, June 16, 2011 Content: 1) Introduction / History 2) Experimental Status
Top rediscovery at ATLAS and CMS
Top rediscovery at ATLAS and CMS on behalf of ATLAS and CMS collaborations CNRS/IN2P3 & UJF/ENSPG, LPSC, Grenoble, France E-mail: julien.donini@lpsc.in2p3.fr We describe the plans and strategies of the
MODERN ATOMIC THEORY AND THE PERIODIC TABLE
CHAPTER 10 MODERN ATOMIC THEORY AND THE PERIODIC TABLE SOLUTIONS TO REVIEW QUESTIONS 1. Wavelength is defined as the distance between consecutive peaks in a wave. It is generally symbolized by the Greek
Light as a Wave. The Nature of Light. EM Radiation Spectrum. EM Radiation Spectrum. Electromagnetic Radiation
The Nature of Light Light and other forms of radiation carry information to us from distance astronomical objects Visible light is a subset of a huge spectrum of electromagnetic radiation Maxwell pioneered
Main properties of atoms and nucleus
Main properties of atoms and nucleus. Atom Structure.... Structure of Nuclei... 3. Definition of Isotopes... 4. Energy Characteristics of Nuclei... 5. Laws of Radioactive Nuclei Transformation... 3. Atom
Big Bang Nucleosynthesis
Big Bang Nucleosynthesis The emergence of elements in the universe Benjamin Topper Abstract. In this paper, I will first give a brief overview of what general relativity has to say about cosmology, getting
arxiv:hep-ph/9808297v1 11 Aug 1998
Testing for New Physics with Low-Energy Anti-Neutrino Sources: LAMA as a Case Study arxiv:hep-ph/9808297v1 11 Aug 1998 I. Barabanov a, R. Bernabei b, O. G. Miranda c V. B. Semikoz d, and J.W.F. Valle c
Measurement of Neutralino Mass Differences with CMS in Dilepton Final States at the Benchmark Point LM9
Measurement of Neutralino Mass Differences with CMS in Dilepton Final States at the Benchmark Point LM9, Katja Klein, Lutz Feld, Niklas Mohr 1. Physikalisches Institut B RWTH Aachen Introduction Fast discovery
Image Processing Techniques applied to Liquid Argon Time Projection Chamber(LArTPC) Data
Image Processing Techniques applied to Liquid Argon Time Projection Chamber(LArTPC) Data Jessica Esquivel On Behalf of the MicroBooNE Collaboration Syracuse University Advisor: Mitch Soderberg Outline
Chem 115 POGIL Worksheet - Week 4 Moles & Stoichiometry Answers
Key Questions & Exercises Chem 115 POGIL Worksheet - Week 4 Moles & Stoichiometry Answers 1. The atomic weight of carbon is 12.0107 u, so a mole of carbon has a mass of 12.0107 g. Why doesn t a mole of
High Precision Measurement of the Target Mass of the Daya Bay Neutrino Detectors
High Precision Measurement of the Target Mass of the Daya Bay Neutrino Detectors Tom Wise on behalf of Daya Bay collaboration Day Bay is a reactor based experiment dedicated to measurement of the last
Precision Electroweak Measurements with the LBNF Near Detector
Precision Electroweak Measurements with the LBNF Near Detector R. Petti University of South Carolina, USA CETUP Near Detector Physics Workshop Deadwood, SD, USA, July 10-21, 2014 MOTIVATIONS A new measurement
KE A = PE MAX 1/2M v 2 = k q1 q2 /R
CHAPTER 13 NUCLEAR STRUCTURE NUCLEAR FORCE The nucleus is help firmly together by the nuclear or strong force, We can estimate the nuclear force by observing that protons residing about 1fm = 10-15m apart
Masses in Atomic Units
Nuclear Composition - the forces binding protons and neutrons in the nucleus are much stronger (binding energy of MeV) than the forces binding electrons to the atom (binding energy of ev) - the constituents
Measurement of Germanium Detector Efficiency
Measurement of Germanium Detector Efficiency Marcus H. Wiggs 2009 Notre Dame Physics REU Advisor: Dr. Philippe Collon Mentors: Matthew Bowers, Daniel Robertson, Chris Schmitt ABSTRACT: A possible discrepancy
Nuclear ZPE Tapping. Horace Heffner May 2007
ENERGY FROM UNCERTAINTY The uncertainty of momentum for a particle constrained by distance Δx is given, according to Heisenberg, by: Δmv = h/(2 π Δx) but since KE = (1/2) m v 2 = (1/(2 m) ) (Δmv) 2 ΔKE
ATLAS NOTE ATLAS-CONF-2010-063. July 21, 2010. Search for top pair candidate events in ATLAS at s = 7 TeV. The ATLAS Collaboration.
ATLAS NOTE ATLAS-CONF-2010-063 July 21, 2010 Search for top pair candidate events in ATLAS at s = 7 TeV The ATLAS Collaboration Abstract A search is performed for events consistent with top quark pair
Light-neutrino mass spectrum, nuclear matrix elements, and the observability of neutrinoless ββ decay
Nuclear Physics A 729 (2003) 867 883 www.elsevier.com/locate/npe Light-neutrino mass spectrum, nuclear matrix elements, and the observability of neutrinoless ββ decay O. Civitarese a,, J. Suhonen b a Department
ORTEC DET-SW-UPG. Latest Software Features. Ease of Use. Source Location with the Detective V3 Software
ORTEC DET-SW-UPG Latest Software Features Three Search Modes: Gamma/Neutron total count rate. SNM search mode. Sliding average "monitor" mode. (NEW) User choice of identification schemes: Classify mode
Chem 115 POGIL Worksheet - Week 4 Moles & Stoichiometry
Chem 115 POGIL Worksheet - Week 4 Moles & Stoichiometry Why? Chemists are concerned with mass relationships in chemical reactions, usually run on a macroscopic scale (grams, kilograms, etc.). To deal with
Basic Concepts in Nuclear Physics
Basic Concepts in Nuclear Physics Paolo Finelli Corso di Teoria delle Forze Nucleari 2011 Literature/Bibliography Some useful texts are available at the Library: Wong, Nuclear Physics Krane, Introductory
NEUTRINO OSCILLATIONS
6 OCTOBER 2015 Scientific Background on the Nobel Prize in Physics 2015 NEUTRINO OSCILLATIONS compiled by the Class for Physics of the Royal Swedish Academy of Sciences THE ROYAL SWEDISH ACADEMY OF SCIENCES,
CHROMOSPHERIC DYNAMICS FROM RHESSI AND RESIK DATA
CHROMOSPHERIC DYNAMICS FROM RHESSI AND RESIK DATA T. Mrozek 1,2, S. Kołomański 2,B. Sylwester 1, A. Kępa 1, J. Sylwester 1, S. Gburek 1, M. Siarkowski 1, M. Gryciuk 1, M. Stęślicki 1 1 Solar Physics Division,
Calorimetry in particle physics experiments
Calorimetry in particle physics experiments Unit n. 8 Calibration techniques Roberta Arcidiacono Lecture overview Introduction Hardware Calibration Test Beam Calibration In-situ Calibration (EM calorimeters)
The Compact Muon Solenoid Experiment. CMS Note. Mailing address: CMS CERN, CH-1211 GENEVA 23, Switzerland. D. J. Mangeol, U.
Available on CMS information server CMS NOTE 6/96 The Compact Muon Solenoid Experiment CMS Note Mailing address: CMS CERN, CH11 GENEVA 3, Switzerland July, 6 Search for χ decays to ττ and SUSY mass spectrum
EDXRF of Used Automotive Catalytic Converters
EDXRF of Used Automotive Catalytic Converters Energy Dispersive X-Ray Fluorescence (EDXRF) is a very powerful technique for measuring the concentration of elements in a sample. It is fast, nondestructive,
Name period AP chemistry Unit 2 worksheet Practice problems
Name period AP chemistry Unit 2 worksheet Practice problems 1. What are the SI units for a. Wavelength of light b. frequency of light c. speed of light Meter hertz (s -1 ) m s -1 (m/s) 2. T/F (correct
Data Provided: A formula sheet and table of physical constants is attached to this paper. DARK MATTER AND THE UNIVERSE
Data Provided: A formula sheet and table of physical constants is attached to this paper. DEPARTMENT OF PHYSICS AND ASTRONOMY Autumn Semester (2014-2015) DARK MATTER AND THE UNIVERSE 2 HOURS Answer question
A new energy source from nuclear fusion
A new energy source from nuclear fusion S. Focardi (1) and A. Rossi (2) (1) Physics Department Bologna University and INFN Bologna Section (2) Leonardo Corp. (USA) - Inventor of the Patent April 22, 2010
ITN network : CNRS Node
ITN network : CNRS Node Invisibles Pre-Meeting, Madrid, 29-30 March 2012 Asmaa Abada Orsay Saclay Lyon Clermont Grenoble LPT IPhT IPNL LPC LPSC Laboratories and People Orsay Laboratoire de Physique Théorique:
Modified Gravity and the CMB
Modified Gravity and the CMB Philippe Brax, IphT Saclay, France arxiv:1109.5862 PhB, A.C. Davis Work in progress PhB, ACD, B. Li Minneapolis October 2011 PLANCK will give us very precise information on
Professional Liability Errors and Omissions Insurance Application
If coverage is issued, it will be on a claims-made basis. Notice: this insurance coverage provides that the limit of liability available to pay judgements or settlements shall be reduced by amounts incurred
Gravitational waves from neutron stars binaries: accuracy and tidal effects in the late inspiral S. Bernuzzi TPI-PAF FSU Jena / SFB-TR7
Gravitational waves from neutron stars binaries: accuracy and tidal effects in the late inspiral S. Bernuzzi TPI-PAF FSU Jena / SFB-TR7 M. Thierfelder, SB, & B.Bruegmann, PRD 84 044012 (2011) SB, MT, &
Weak Interactions: towards the Standard Model of Physics
Weak Interactions: towards the Standard Model of Physics Weak interactions From β-decay to Neutral currents Weak interactions: are very different world CP-violation: power of logics and audacity Some experimental
Dark Energy, Modified Gravity and The Accelerating Universe
Dark Energy, Modified Gravity and The Accelerating Universe Dragan Huterer Kavli Institute for Cosmological Physics University of Chicago Makeup of universe today Dark Matter (suspected since 1930s established
The ANGRA Neutrino Project
The ANGRA Neutrino Project Ernesto Kemp kemp@ifi.unicamp.br State University at Campinas - UNICAMP Gleb Wataghin Physics Institute Cosmic Rays and Chronology Department 14/12/2007 E.Kemp - Encontro CBPF
ASACUSA: Measuring the Antiproton Mass and Magnetic Moment
Dezső Horváth ASACUSA ECFA, 4 October 2013, Wigner FK, Budapest p. 1/19 ASACUSA: Measuring the Antiproton Mass and Magnetic Moment Dezső Horváth on behalf of the ASACUSA Collaboration horvath.dezso@wigner.mta.hu
arxiv:hep-ex/0203014v1 8 Mar 2002
Cosmogenesis Backgrounds, Experiment Depth and the Solar Neutrino TPC G. Bonvicini, A. Schreiner arxiv:hep-ex/0203014v1 8 Mar 2002 Abstract Wayne State University, Detroit MI 48201 A Time Projection Chamber