Sterile neutrinos. Stéphane Lavignac (IPhT Saclay)
|
|
- Brent Bond
- 5 years ago
- Views:
Transcription
1 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 9ème Rencontre SPP/IPhT: Les neutrinos Saclay, 4 janvier 01
2 Introduction Several oscillation results or anomalies (reactor antineutrino anomaly, LSND ν µ ν e data...) cannot be explained within 3-flavour oscillations need at least a fourth neutrino But constraint from the invisible decay width of the Z boson [LEP]: N ν =.9840 ± additional neutrinos must be sterile (i.e. electroweak singlets) or be heavier than MZ / Sterile neutrinos are SM gauge singlets - only interact via their mixing with the active neutrinos oscillations ν e,µ,τ ν s Other motivations for sterile neutrinos from cosmology, e.g. kev sterile neutrino as warm dark matter [Shaposhnikov] or to explain pulsar velocities [Kusenko, Segrè]
3 Standard case (3 flavours): Active-sterile neutrino mixing Add a sterile neutrino: ν α = 4 i=1 U flavour eigenstate αi ν i [ α = e, µ, τ ] U = 4x4 unitary matrix ν e,ν µ,ν τ mass eigenstate (m4) Only couple to electroweak gauge boson, but all four mass eigenstate are produced in a beta decay: e ν e = 4 i=1 U ei ν i ν s ν 4
4 -flavour oscillations: ( m P (ν α ν β ) = sin θ sin ) L ( να ν β ) ( cos θ sin θ = sin θ cos θ )( ν1 ν ) m m m 1 N-flavour oscillations: P να ν β ( ν α ν β ) = δ αβ 4 i<j i<j Re ( U αi U βiu αju βj ) sin ( ) m ij L Im ( ( ) U αi UβiU αju ) m ij L βj sin E
5 3+1 case: Since m SBL m atm., m sun, it is natural (and cosmologically preferred) to assume m 4 m 3,m,m 1 Then m SBL m 41 m 4 m 43 all other m ij s All data but short baseline oscillations well described by 3-flavour oscillations ν 1,,3 mainly composed of ν e,µ,τ + small admixture of ν s, and mainly composed of + small admixture of ν 4 ν s ν e,µ,τ! $ Smirnov %&'' $% ",-./! +! "!# $% " &(% $% " ')*
6 We are interested in short baseline oscillations with m 41L P να ν α ( ) m 1 = sin 41 L ( ) m sin 31 L, sin ( m 1 L 1 4 ( U α1 + U α + U α3 ) ( ) m U α4 sin 41 L ( ) m 1 sin θ αα sin 41 L ) where P να ν β where sin θ αα 4 (1 U α4 ) U α4 4 Re [( U α1 Uβ1 + U α Uβ + U α3 Uβ3 ( ) m sin θ αβ sin 41 L sin θ αβ 4 U α4 U β4 ( ) ) ] U α4 U β4 sin m 41 L
7 3+ case: Assume m 5 m 4 m 3,m,m 1 two relevant squared mass differences m 51 and m 41 CP-violating effects possible due to interference between the two oscillations frequencies P να ν β ( ν α ν β ) η arg [ U α4 U β4u α5u β5 ] ( ) ( ) m = 4 U α4 U β4 sin 41 L m +4 U α5 U β5 sin 51 L ( ) ( ) ( m +8 U α4 U β4 U α5 U β5 sin 41 L m sin 51 L m cos 54 L ) η
8 Cosmological constraints Light sterile neutrinos are in thermal equilibrium in the early universe due to oscillations (unless small active-sterile mixing) increase the number of relativistic species affect BBN, CMB anisotropies and large-scale structure formation Hamann, Hannestad, Raffelt, Wong [ ]: within ΛCDM, CMB+LSS and BBN prefer extra relativistics dofs: N eff = (95% C.L.) However, a sterile neutrino with an ev mass violates the cosmological bound on neutrino masses m ev or must depart from ΛCDM: e.g. additional relativistic dofs help relax this bound, but inconsistent with BBN (allows at most one extra relativistic dof) unless introduce a neutrino chemical potential If ev-scale sterile neutrinos are really around, seem to require a significant modification of the standard cosmological scenario
9 Experimental situation Several experimental anomalies suggest the existence of sterile neutrinos LSND: oscillations Excess of ν e events over background at 3.8 σ (still controversial) Not observed by KARMEN MiniBooNE: ν µ ν e ν e ν µ ν e data: no excess in the MeV range, but unexplained 3σ excess at low energy ν µ ν e ν e data: excess in the E > 475 MeV region consistent with LSND-like oscillations, but also (after the 011 update) with a background-only hypothesis A low-energy excess is also seen ν e ) 4 /c (ev m 1-1 LSND 90% C.L. LSND 99% C.L. sin (θ) upper limit MiniBooNE 90% C.L.y MiniBooNE 90% C.L. sensitivity BDT analysis 90% C.L sin (θ) -1 1
10 Reactor antineutrino anomaly: New computation of the reactor antineutrino spectra increase of the flux by about 3% deficit of antineutrinos in SBL reactor experiments mean observed to predicted rate ± N OBS /(N EXP ) pred,new ILL Bugey!3 Bugey!4 ROVNO88!1S ROVNO88!3S ROVNO91 ROVNO88!I SRP!I ROVNO88!1I SRP!II ROVNO88!S Krasnoyarsk!I Goesgen!I Bugey!3 Goesgen!II Krasnoyarsk!III Goesgen!III Krasnoyarsk!II Bugey!3 PaloVerde CHOOZ G. Mention et al. 1 3 Distance to Reactor (m) FIG. 5. Illustration of the short baseline reactor antineutrino anomaly. The experimental results are compared to the prediction without oscillation, taking into account the new antineutrino spectra, the corrections of the neutron mean lifetime, and the off-equilibrium effects. Published experimental errors and antineutrino spectra errors are added in quadrature. The mean averaged ratio including possible correlations is ± The red line shows a possible 3 active neutrino mixing solution, with sin (θ 13 ) = The blue line displays a solution including a new neutrino mass state, such as m new,r 1 ev and sin (θ new,r ) = 0.1 (for illustration purpose only).
11 Gallex-SAGE calibration experiments: Calibration of the Gallex and SAGE experiments with radioactive sources observed deficit of ν e with respect to predictions R = 0.86 ± 0.05 [tension with ν e - Carbon cross-section measurements at LSND and KARMEN, ] Combined analysis of SBL reactor data, gallium calibration experiments and MiniBooNE neutrino data [G. Mention et al.]: m SBL > 1.5 ev, sin θ ee =0.14 ± 0.08 (95% C.L.)
12 However, no coherent picture of the data with an additional (or even ) sterile neutrinos (even if the global fit has improved with the new reactor antineutrino flux): 1) tension between appearance (LSND/MiniBooNE antineutrino data) and disappearance experiments (reactors, ν µ disappearence experiments) ( ) m Reactors: P νe ν e 1 sin θ ee sin 41 L require relatively small CDHS: P νµ ν µ sin θ ee 4 (1 U e4 ) U e4 4 U e4 (using info from solar neutrino data) ( ) m 1 sin θ µµ sin 41 L require relatively small sin θ µµ 4 (1 U µ4 ) U µ4 4 U µ4 (using info from atm. neutrino data)
13 Appearance experiments (LSND/MiniBooNE antineutrino data): ( ) m P νµ ν e sin θ eµ sin 41 L sin θ eµ 4 U e4 U µ4 1 4 sin θ ee sin θ µµ 99% C.L. Bugey!3 (1995) Bugey!4 (1994) + Rovno (1991) Gosgen (1986) + ILL (1995) Krasnoyarsk (1994) 99% C.L. Reactors CDHSW + Atm Disappearance LSND + MB$ [ev ] "m 41 [ev ] [ev ] #1 "m 41 #1 "m 41 #1 # # #1 1 sin! ee 99% C.L. CDHSW (1984): $ µ ATM: $ µ + $ µ # # #1 1 sin! µµ # #4 #3 # #1 1 sin! eµ Giunti,
14 ) tension between LSND and MiniBooNE neutrino data (+ null result of NOMAD and KARMEN) Giunti, "m 41 [ev ] #1 99% C.L. MB$ + LSND$ Dis + KAR + NOM + MB$ # #4 #3 # #1 1 1 MB# KARMEN NOMAD sin! eµ "m 41 [ev ] 0 disappearance LSND + MB# $ 90, 99% CL Kopp, Maltoni, Schwetz, % CL ( dof) sin! SBL
15 3+1 case does not provide a very satisfactory fit of all the data Best fit point of a global analysis [Giunti, Laveder, incl. MiniBooNE 011]: m 41 =1.6eV, U e4 =0.036, U µ4 = [ sin θ eµ =1. 3] 3+ case [Kopp, Maltoni, Schwetz] Allows for CP violation can reconcile MiniBooNE neutrino data with LSND/MiniBooNE 0 antineutrino data (less motivated after inclusion of 011 data) LSND Much better fit of pre-011 data than in the 3+1 case [low-energy excess of MiniBooNE not included in the fit] P ( ν µ ν e ) P (ν µ ν e ) excess events P LSND [%] MiniBooNE (neutrinos) MiniBooNE (anti-neutrinos) E # CCQE [GeV] E # CCQE [GeV]
16 Other implications of sterile neutrinos Tritium beta decay: 3 H 3 H e + e + ν e E 0 = m 3 H m 3 H e The electron energy spectrum is given by: dn = R(E e ) (E 0 E e ) de m ν E e = E 0 E ν e Effect of the non-vanishing neutrino mass: Ee max = E 0 E 0 m ν distorsion of the Ee spectrum close to the endpoint
17 Present bound (Troitsk/Mainz): KATRIN will reach a sensitivity of about 0.3 ev m νe <. ev (95% C.L.) In pratice, there is no electron neutrino mass, but 3 (or more) strongly mixed mass eigenstates, and dn = R(E e ) U ei (E 0 E e ) de m i Θ(E 0 E e m i ) e i If all mi are smaller than the energy resolution, this can be rewritten as: dn = R(E e ) m i U de ei e (E 0 E e ) m β m β i If there is an ev-scale sterile neutrino (comparable to the energy resolution of KATRIN), its mass may be resolved (but difficult measurement): 1 R(E e ) dn = (1 U e4 ) (E 0 E e ) de m β e + U e4 (E 0 E e ) m 4 Θ(E 0 E e m 4 ) (dn/dee) 1/ (also: upper bound on m4 from beta decay) Q! m " H Q! m " L Q E e
18 Neutrinoless double beta decay: (A, Z) (A, Z + ) + e + e Possible if lepton number violated (Majorana neutrinos), in nuclei where the single beta decay is forbidden Sensitive to the effective mass parameter: m ββ i m i U ei possible cancellations in the sum (phases in U) 1 disfavoured by 0ΝΒ 3-neutrino case (Strumia, Vissani) mee in ev CL 1 dof m 3 0 m 3 0 disfavoured by cosmology lightest neutrino mass in ev
19 An additional sterile neutrino will contribute to the effective mass m ββ m 4 U e4 e iγ i m iuei ; depending on the active neutrino parameters it may dominate or lead to cancellations <m ee > (ev) , Normal, SN 1+3, Inverted, SI 3! (best-fit) 3! (") 1+3! (best-fit) 1+3! (") 3! (best-fit) 3! (") 1+3! (best-fit) 1+3! (") Barry, Rodejohann, Zhang, m light (ev) using the fit of Kopp, Maltoni and Schwetz: 3+1/1+3 parameter m 41 [ev] U e4 best-fit σ
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
More informationImpact of light sterile!s in LBL experiments "
Xmas Theory Workshop Bari, 22/12/14 Impact of light sterile!s in LBL experiments " Work done in collaboration with L. Klop (Master Thesis at MPI) (now PhD student @ GRAPPA Institute, Amsterdam) Antonio
More informationTwo 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
More informationSterile 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,
More informationOscillations 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
More informationSterile 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
More informationSterile 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,
More informationStatus 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
More informationNeutrino 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
More informationStatus of Sterile Neutrinos Carlo Giunti
Status of Sterile Neutrinos 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 NOW 0, Neutrino
More informationOscillations 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,
More informationThe reactor antineutrino anomaly & experimental status of anomalies beyond 3 flavors
The reactor antineutrino anomaly & experimental status of anomalies beyond 3 flavors G. Mention CEA Saclay / Irfu / SPP Rencontres IPhT-SPP, 24 janvier 2012 Overview List of anomalies: LSND MB, anti- Gallium
More informationCarlo 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
More informationSterile 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
More informationNeutrino 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
More informationC. 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
More informationAnalysis 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
More informationNeutrino 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
More informationNeutrino 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
More informationOn 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
More informationNeutrinos & Large Extra Dimensions. Renata Zukanovich Funchal Universidade de São Paulo, Brazil
Neutrinos & Large Extra Dimensions Renata Zukanovich Funchal Universidade de São Paulo, Brazil What is ν? Workshop June 26, 2012 ν Masses & Mixings Majorana CP Violating phases solar atmospheric accelerator
More informationNeutrino Phenomenology. Boris Kayser ISAPP July, 2011 Part 1
Neutrino Phenomenology Boris Kayser ISAPP July, 2011 Part 1 1 What Are Neutrinos Good For? Energy generation in the sun starts with the reaction Spin: p + p "d + e + +# 1 2 1 2 1 1 2 1 2 Without the neutrino,
More informationReactor anomaly and searches of sterile neutrinos in experiments at very short baseline
Reactor anomaly and searches of sterile neutrinos in experiments at very short baseline G. MENTION CEA Saclay Irfu / SPP Workshop Inνisibles 13 July 17 th, 2013 Content Is the standard 3 neutrino mixing
More informationFlavor Models with Sterile Neutrinos. NuFact 11 Geneva, Aug, He Zhang
Flavor Models with Sterile Neutrinos NuFact 11 Geneva, Aug, 2011 Contents: Sterile neutrinos in ν-osc. and 0νββ decays Mechanisms for light sterile neutrino masses Flavor symmetry with sterile neutrinos
More informationNeutrino Anomalies & CEνNS
Neutrino Anomalies & CEνNS André de Gouvêa University PIRE Workshop, COFI February 6 7, 2017 Something Funny Happened on the Way to the 21st Century ν Flavor Oscillations Neutrino oscillation experiments
More informationNeutrino 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
More informationStatus 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
More informationHow many neutrino species are there?
How many neutrino species are there? Jan Hamann 6. Kosmologietag, Bielefeld 5-6 May 2011 Radiation content of the Universe Microwave background Neutrino background standard model expectation: [Mangano
More informationSterile neutrinos: to be or not to be?
Sterile neutrinos: to be or not to be? Joachim Kopp (University of Mainz) June 9, 2015 @ WIN 2015, Heidelberg Joachim Kopp Sterile neutrinos: to be or not to be? 1 Outline 1 Sterile Neutrinos 2 Oscillation
More informationShort-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
More informationSterile Neutrinos from the Top Down
Sterile Neutrinos from the Top Down Active-sterile mixing The landscape Small Dirac or Majorana masses (or both) The mini-seesaw Light Sterile Neutrinos: A White Paper (K. Abazajian et al), 1204.5379 Neutrino
More informationNeutrino Phenomenology. Boris Kayser INSS August, 2013 Part 1
Neutrino Phenomenology Boris Kayser INSS August, 2013 Part 1 1 What Are Neutrinos Good For? Energy generation in the sun starts with the reaction Spin: p + p "d + e + +# 1 2 1 2 1 1 2 1 2 Without the neutrino,
More informationStefano Gariazzo. Light sterile neutrino: the 2018 status. IFIC, Valencia (ES) CSIC Universitat de Valencia
Stefano Gariazzo IFIC, Valencia (ES) CSIC Universitat de Valencia gariazzo@ific.uv.es http://ific.uv.es/~gariazzo/ Light sterile neutrino: the 08 status The Magnificent CEνNS, Chicago, 03//08 Neutrino
More informationNeutrinos 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
More informationev-scale Sterile Neutrinos
ev-scale Sterile Neutrinos Carlo Giunti 1 and Thierry Lasserre 2 1 Istituto Nazionale di Fisica Nucleare (INFN), Sezione di Torino, Via P. Giuria 1, I 10125 Torino, Italy; email: carlo.giunti@to.infn.it
More informationarxiv: v1 [hep-ph] 15 Apr 2019
International Journal of Modern Physics A c World Scientific Publishing Company arxiv:1904.07108v1 [hep-ph] 15 Apr 2019 Roles of sterile neutrinos in particle physics and cosmology Sin Kyu Kang School
More informationStatus 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
More informationThermalisation of Sterile Neutrinos. Thomas Tram LPPC/ITP EPFL
Thermalisation of Sterile Neutrinos Thomas Tram LPPC/ITP EPFL Outline Introduction to ev sterile neutrinos. Bounds from Cosmology. Standard sterile neutrino thermalisation. Thermalisation suppression by
More informationSterile Neutrinos from the Top Down
Sterile Neutrinos from the Top Down Active-sterile mixing The landscape Small Dirac/Majorana masses The mini-seesaw Light Sterile Neutrinos: A White Paper (K. Abazajian et al), 1204.5379 Neutrino Masses
More informationNeutrino Oscillations And Sterile Neutrinos
Neutrino Oscillations And Sterile Neutrinos Keshava Prasad Gubbi University of Bonn s6nagubb@uni-bonn.de May 27, 2016 Keshava Prasad Gubbi (Uni Bonn) Neutrino Oscillations,Sterile Neutrinos May 27, 2016
More informationHint 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
More informationThe Physics of Neutrino Oscillation. Boris Kayser INSS August, 2013
The Physics of Neutrino Oscillation Boris Kayser INSS August, 2013 1 Neutrino Flavor Change (Oscillation) in + l α (e.g. µ) Vacuum ( Approach of ) B.K. & Stodolsky - l β (e.g. τ) Amp ν W (ν α ) (ν β )
More informationExotic Charges, Multicomponent Dark Matter and Light Sterile Neutrinos
Exotic Charges, Multicomponent and Light Sterile Neutrinos Julian Heeck Max-Planck-Institut für Kernphysik, Heidelberg 2.10.2012 based on J.H., He Zhang, arxiv:1210.xxxx. Sterile Neutrinos Hints for ev
More informationIntroduction to Neutrino Physics. TRAN Minh Tâm
Introduction to Neutrino Physics TRAN Minh Tâm LPHE/IPEP/SB/EPFL This first lecture is a phenomenological introduction to the following lessons which will go into details of the most recent experimental
More informationNeutrinos 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
More informationNeutrinos and Astrophysics
Neutrinos and Astrophysics Astrophysical neutrinos Solar and stellar neutrinos Supernovae High energy neutrinos Cosmology Leptogenesis Big bang nucleosynthesis Large-scale structure and CMB Relic neutrinos
More informationOverview 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
More informationMiniBooNE, 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
More informationThe Physics of Neutrino Oscillation
The Physics of Neutrino Oscillation Boris Kayser PASI March, 2012 1 Neutrino Flavor Change (Oscillation) in Vacuum + l α (e.g. µ) ( ) Approach of B.K. & Stodolsky - l β (e.g. τ) Amp W (ν α ) (ν β ) ν W
More informationSterile neutrinos at future long-baseline experiments
Davide Meloni, Dip. Fisica Roma Tre & INFN sez. Roma Tre, Friday 12, NOW 2008 1 Introduction Sterile neutrinos today 2 Current limits on new mixing angles The question of the parameterization Current allowed
More informationThe Hunt for Sterile Neutrinos. H. Ray, University of Florida
The Hunt for Sterile Neutrinos 1 Particle Physics is Over!..finding the Higgs arguably the most important discovery in more than a generation has left physicists without a clear roadmap of where to go
More informationMarch 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:
More informationNeutrinos secretly converting to lighter particles to please both KATRIN and Cosmos. Yasaman Farzan IPM, Tehran
Neutrinos secretly converting to lighter particles to please both KATRIN and Cosmos Yasaman Farzan IPM, Tehran Outline Motivation for the KATRIN experiment Effect of neutrinos on cosmological scales and
More informationWhat 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
More informationNOW Conca Specchiulla, September 9-16, 2012
Conca Specchiulla, September 9-16, 2012 NOW 2012!"#$%&'(%)*+%,-%.()*-/,/'"*++0#/-',*-, (1%,20)+3,4-*$%)'%,5*(1,63-07*"0+, -%.()*-/,0'377%()*%',, Ninetta Saviano II Institut für Theoretische Physik, Universität
More informationNeutrino Physics After the Revolution. Boris Kayser PASI 2006 October 26, 2006
Neutrino Physics After the Revolution Boris Kayser PASI 2006 October 26, 2006 1 What We Have Learned 2 The (Mass) 2 Spectrum ν 3 ν 2 ν 1 } Δm 2 sol (Mass) 2 Δm 2 atm or Δm 2 atm ν ν 2 } Δm 2 sol 1 ν 3
More informationOn indications for sterile neutrinos at the ev scale. Invisibles 14 workshop, July 2014, Paris Thomas Schwetz
On indications for sterile neutrinos at the ev scale Invisibles 14 workshop, 14-18 July 014, Paris Thomas Schwetz 1 Anomalies at the E/L ~ ev scale Reactor anomaly (νe disappearance) Gallium anomaly (νe
More informationGLOBAL ANALYSIS OF NEUTRINO DATA
GLOBAL ANALYSIS OF NEUTRINO DATA Stony Brook & IFIC-Valencia) Nobel Syposiu, August 4 Introduction: The Paraeters of the New Minial Standard Model Orthodox Global Fits Solar and Reactor Neutrinos Atospheric
More informationarxiv: v2 [hep-ph] 31 Aug 2010
EURONU-WP6-1-24 MiniBooNE and LSND data: non-standard neutrino interactions in a (3+1) scheme versus (3+2) oscillations arxiv:17.4171v2 [hep-ph] 31 Aug 21 Evgeny Akhmedov 1,2, and Thomas Schwetz 1, 1 Max-Planck-Institut
More informationParticle 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
More informationNeutrinos. 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
More informationThe Reactor Antineutrino Anomaly
The Reactor Antineutrino Anomaly M. Fechner, G. Mention, T. Lasserre, M. Cribier, Th. Mueller D. Lhuillier, A. Letourneau, CEA / Irfu arxiv:1101.2755 [hep-ex] Introduction New spectra calculations presented
More informationGrand 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
More informationNeutrinos in Supernova Evolution and Nucleosynthesis
Neutrinos in Supernova Evolution and Nucleosynthesis Gabriel Martínez Pinedo The origin of cosmic elements: Past and Present Achievements, Future Challenges, Barcelona, June 12 15, 2013 M.-R. Wu, T. Fischer,
More informationUnbound 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 ±
More informationCosmological constraints on the Sessaw Scale
Cosmological constraints on the Sessaw Scale Jacobo López-Pavón 50th Rencontres de Moriond EW La Thuile, Valle d'aosta (Italy) 14-21 March, 2015 Motivation Which is the simplest extension of the SM that
More informationOverview of Reactor Neutrino
Overview of Reactor Neutrino Chan-Fai (Steven) Wong, Wei Wang Sun Yat-Sen University 22 September 2016 The 14th International Workshop on Tau Lepton Physics Many thanks to Jia Jie Ling, Liang Jian Wen
More informationNEUTRINO 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
More informationWhy neutrinos? Patrick Huber. Center for Neutrino Physics at Virginia Tech. KURF Users Meeting June 7, 2013, Virginia Tech. P. Huber VT-CNP p.
Why neutrinos? Patrick Huber Center for Neutrino Physics at Virginia Tech KURF Users Meeting June 7, 2013, Virginia Tech P. Huber VT-CNP p. 1 Neutrinos are massive so what? Neutrinos in the Standard Model
More informationSearching for Physics Beyond the Standard Model with Accelerator ν Experiments W.C Louis, LANL. MiniBooNE Status FNAL ORNL
Searching for Physics Beyond the Standard Model with Accelerator ν Experiments W.C Louis, LANL MiniBooNE Status BooNE @ FNAL OscSNS @ ORNL Happy 75 th Birthdays to Frank Avignone, Ettore Fiorini, & Peter
More informationImplications of cosmological observables for particle physics: an overview
Implications of cosmological observables for particle physics: an overview Yvonne Y. Y. Wong The University of New South Wales Sydney, Australia TAUP 2015, Torino, September 7 11, 2015 The concordance
More informationNeutrino 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
More informationNeutrino 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:
More informationStefano Gariazzo. Light sterile neutrinos with pseudoscalar interactions in cosmology. Based on [JCAP 08 (2016) 067] University and INFN, Torino
Stefano Gariazzo University and INFN, Torino gariazzo@to.infn.it http://personalpages.to.infn.it/~gariazzo/ Light sterile neutrinos with pseudoscalar interactions in cosmology Based on [JCAP 08 (2016)
More informationarxiv: v2 [hep-ex] 2 Aug 2017
Sterile Neutrinos: An Introduction to Experiments J.M. Conrad 1 and M.H. Shaevitz 2 1 Massachusetts Institute of Technology, Cambridge, MA 2 Columbia University, New York, NY arxiv:1609.07803v2 [hep-ex]
More informationSensitivity 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.
More informationNeutrino Physics. NASA Hubble Photo. Boris Kayser PASI March 14-15, 2012 Part 1
Neutrino Physics NASA Hubble Photo Boris Kayser PASI March 14-15, 2012 Part 1 1 What Are Neutrinos Good For? Energy generation in the sun starts with the reaction Spin: p + p "d + e + +# 1 2 1 2 1 1 2
More informationSterile Neutrinos. Patrick Huber. Center for Neutrino Physics Virginia Tech
Sterile Neutrinos Patrick Huber Center for Neutrino Physics Virginia Tech XIII Workshop on Electron-Nucleus Scattering June 23-27, 2014, Marciana Marina, Isola d Elba, Italy P. Huber p. 1 Outline The reactor
More informationSNOW 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
More informationNeutrino 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
More informationDark Radiation and Inflationary Freedom
Dark Radiation and Inflationary Freedom Based on [SG et al., JCAP 1504 (2015) 023] [Di Valentino et al., PRD 91 (2015) 123505] Stefano Gariazzo University of Torino, INFN of Torino http://personalpages.to.infn.it/~gariazzo/
More informationMinimal Extension of the Standard Model of Particle Physics. Dmitry Gorbunov
Minimal Extension of the Standard Model of Particle Physics Dmitry Gorbunov Institute for Nuclear Research, Moscow, Russia 14th Lomonosov Conference on Elementary Paticle Physics, Moscow, MSU, 21.08.2009
More informationCritical Review on Neutrino Anomalies. Carlo Giunti
C. Giunti Review on Neutrino Anomalies Neutrinos: the Quest for a New Physics Scale 7 March 07 /49 Critical Review on Neutrino Anomalies Carlo Giunti INFN, Torino, Italy Neutrinos: the Quest for a New
More informationKnown and Unknown for Neutrinos. Kim Siyeon Chung-Ang g University Lecture at Yonsei Univ.
Known and Unknown for Neutrinos Kim Siyeon Chung-Ang g University Lecture at Yonsei Univ. Known and Unknown for Neutrinos Dirac vs. Majorana 3 generation vs. 4 generation (neutrino vs. antineutrino) (terrestrial
More informationNeutrino properties: nature, mass & CP violation
Neutrino properties: nature, mass & CP violation I. Schienbein LPSC prepared together with P. Serpico (LAPTH) and A. Wingerter (LPSC) Kick-off meeting, 2/0/202, Annecy Facts of life with neutrinos Neutrino
More informationSun Yat-Sen University, 135 Xingang Xi Road, Guangzhou, Guangdong, , China
Sun Yat-Sen University, 135 Xingang Xi Road, Guangzhou, Guangdong, 510275, China E-mail: lingjj5@mail.sysu.edu.cn The basic theory and experimental hints for light sterile neutrinos at ev 2 mass scale
More informationParticle 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
More information1 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.
More informationNeutrinos: 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
More informationThe 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
More informationGeV neutrino mass models: Experimental reach vs. theoretical predictions RWR, Walter Winter Arxiv PRD 94, (2016)
GeV neutrino mass models: Experimental reach vs. theoretical predictions RWR, Walter Winter Arxiv 1607.07880 PRD 94, 073004 (016) Rasmus W. Rasmussen Matter and the Universe 1-1-16 Theory of elementary
More informationHow large is the "LSND anomaly"?
How large is the "LSND anomaly"? Andrey Elagin on behalf of the HARP-CDP group HEP lunch, UChicago, March 12, 2012 Outline 3.8 σ LSND Final Paper PRD 64, 112007 3.8 σ 2.9 σ HARP-CDP Paper I arxiv:1110.4265
More informationNeutrino 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
More informationReactor Anomaly an Overview. Petr Vogel, Caltech INT Seattle 11/6/2013
Reactor Anomaly an Overview Petr Vogel, Caltech INT Seattle 11/6/2013 in ν e + p -> e + + n Illustration of the reactor anomaly. Rates in various experiments are compared with the expectations based on
More informationMINOS 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
More informationSearch 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
More informationShort baseline experiments and sterile neutrinos. Nick van Remortel Solvay-Francqui Workshop on Neutrinos May
Short baseline experiments and sterile neutrinos Nick van Remortel Solvay-Francqui Workshop on Neutrinos May 27-29 2015 2 Overview Tensions with 3 neutrino paradigm by range of experiments sterile neutrinos
More informationPhenomenological Status of Neutrino Mixing
Phenomenological Status of Neutrino Mixing 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
More informationChapter 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
More informationNeutrinos. Riazuddin National Centre for Physics Quaid-i-Azam University Campus. Islamabad.
Neutrinos Riazuddin National Centre for Physics Quaid-i-Azam University Campus Islamabad. Neutrino was the first particle postulated by a theoretician: W. Pauli in 1930 to save conservation of energy and
More information