Tau Neutrino Physics Introduction. Barry Barish 18 September 2000

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1 Tau Neutrino Physics Introduction Barry Barish 18 September 2000

2 ν τ the third neutrino

3 The Number of Neutrinos big-bang nucleosynthesis D, 3 He, 4 He and 7 Li primordial abundances abundances range over nine orders of magnitude Y < 0.25 from number of neutrons when nucleosynthesis began (Y is the 4 He fraction) Y observed = 0.238±0.002±0.005 presence of additional neutrinos would at the time of nucleosynthesis increases the energy density of the Universe and hence the expansion rate, leading to larger Y. Y BBN = N ν 1.7 N ν 4.3

4 The Number of Neutrinos collider experiments most precise measurements come from Z e + + e invisible partial width, Γ inv, determined by subtracting measured visible partial widths (Z decays to quarks and charged leptons) from the Z width invisible width assumed to be due to N ν Standard Model value (Γ ν Γ ) l SM = ± (using ratio reduces model dependence) N ν = Γ Γ inv l Γl Γ ν SM Nν = ±0.008

5 existence Existence was indirectly established from decay data combined with reaction data (FELDMAN 81). DIRECT EVIDENCE WAS PRESENTED THIS SUMMER FROM FNAL DONUT EXPERIMENT Observe the τ and its decays from ν τ charged current interactions

6 existence DONUT concept calculated number of interactions = 1100 ( ν µ, ν e, ν τ ) total protons on target = data taken from April to September 1997

7 existence DONUT detectors Spectrometer Emulsion-Vertex Detectors

8 existence DONUT detectors triggers yield 203 candidate events

9 existence DONUT events/background 4 events observed 4.1 ± 1.4 expected 0.41± 0.15 background

10 J = ½ J = 3/2 ruled out by establishing that H ± -1 helicity state in τ ρ ν τ magnetic moment expect µ ν = 0 for Majorana or chiral massless Dirac neutrinos extending SU(2)xU(1) for massive neutrinos, ( ) 2 ( 19 8π 2 = ) m B µ ν = 3 Fmν / ν eg µ where mν is in ev and µ B = eh/2m e Bohr magnetons. using upper bound m τ < 35 ΜeV µ ν < µ Β Experimental Bound < µ Β from ν τ e ν τ e

11 electric dipole moment < e cm from Γ(Z ee) at LEP ν τ charge < from Luminosity of Red Giants (Raffelt) lifetime > sec/ev Astrophysics (Bludman) for m ν < 50 ev

12 direct mass measurements Direct bounds come from reconstruction of τ multihadronic decays LEP (Aleph) from 2939 events τ 2π + π + + ν τ < 22.3 MeV/c 2 and 52 events τ 3π + 2π + + (π 0 ) + ν τ < 21.5 MeV/c 2 combined limit < 18.2 MeV/c 2

13 direct mass measurements method two body decay τ (Ε τ,p τ ) h (E h,p h ) + ν τ (Ε ν,p ν ) tau rest frame hadronic energy Ε h = (m τ 2 + m h2 +m ν2 ) / 2m τ laboratory frame E h = γ (E h* + β p h * cosθ) interval bounded for different m ν E h max,min = γ (E h* ± β p h* ) two sample events τ 3π + 2π + + (π 0 ) + ν τ

14 direct mass measurements events & contours 0 MeV/c 2 and 23 MeV/c 2 Log-likelihood fit vs m ν

15 direct mass measurements + cosmological bounds Unstable ν τ bounds on m ν τ from cosmology combined with non observation of lepton number violating decay and direct mass limits

16 mass difference neutrino oscillations neutrinos produced in hadronic cascade of the primary cosmic ray interacting in the atmosphere atmospheric neutrinos at low energies about twice as many muon neutrinos relative to electron neutrinos (error ~ 5%) hint #1 ratio lower than expected Path length from ~20km to km (from below)

17 mass difference neutrino oscillations cosmic ray + atmospheric nucleus mostly 's π s (some K, charm..) π ν µ + µ and µ ν µ + ν e + e yields approximately, µ( 66%) and e ( 33%) ratio-of-ratios: R = (ν µ /ν e ) obs / (ν µ /ν e ) pred

18 mass difference neutrino oscillations Hint #2 anisotropy up/down and distortion of the angular distribution of the up-going events Hint #3 anomalies have been found in a consistent way for all energies Detectors can detect internal of external events produced in the rock below the detector 100 MeV to 1 TeV

19 mass difference neutrino oscillations

20 mass difference neutrino oscillations Superkamiokande

21 mass difference neutrino oscillations distortion in angular distributions reduction factor with maximal mixing

22 mass difference neutrino oscillations Superkamiokande

23 mass difference neutrino oscillations

24 mass difference neutrino oscillations MACRO Detector

25 mass difference neutrino oscillations Detector mass ~ 5.3 kton Event Rate: (1) up throughgoing m (ToF) ~160 /y (2) internal upgoing m (ToF) ~ 50/y (3) internal downgoing m (no ToF) ~ 35/y (4) upgoing stopping m (no ToF) ~ 35/y MACRO at Gran Sasso

26 mass difference neutrino oscillations MACRO results

27 mass difference neutrino oscillations Probabilities of ν µ ν τ oscillations (for maximal mixing) the peak probability from the angular distribution agrees with the peak probability from the total number of events probability for no-oscillation: ~ 0.4 %

28 mass difference neutrino oscillations Probabilities for sterile neutrino oscillations with maximum mixing peak probabilities lower than that for tau neutrinos: from the angular distribution 4.1 % from combination: 14.5 %

29 mass difference neutrino oscillations ratio (Lipari- Lusignoli, Phys Rev D ) can be statistically more powerful than a χ 2 test: 1) the ratio is sensitive to the sign of the deviation 2) there is gain in statistical significance disadvantage: the structure in the angular distribution of data can be lost. ν µ ν τ oscillation favoured with large mixing angle: m 2 ~ 2.5x10-3 ev 2 sterile ν disfavoured at ~ 2 σ level test of oscillations the ratio vertical / horizontal

30 mass difference neutrino oscillations Superkamiokande excluded regions using combined analysis of low energy and high energy data Sobel ν2000 stated.

31 ν τ future speculations - supernovae direct ev scale measurements of m(ν µ ) and m(ν τ ) from Supernovae neutrinos early black hole formation in collapse will truncate neutrino production giving a sharp cutoff allows sensitivity to m(ν e ) ~1.8 ev for SN at 10 kpc in Superkamiokande detector (Beacom et al hep-ph/ ) Events in SK Low: 0 < E < 11.3 MeV mid: 11.3 < E < 30 MeV High: 30 < E <

32 ν τ future speculations - supernovae rate in OMNIS, a proposed supernovae detector OMNIS delayed counts vs mass tail: 6.1 ev 2.3 events

33 ν τ future speculations cosmic ν τ s high energy ν s E > 10 6 GeV neutrinos from proton acceleration in the cores of active galactic nuclei vacuum flavor neutrino oscillations enhance ν τ / ν µ ratio detectable in under water / under ice detectors (Athar et al hep-ph/ )

34 ν τ future speculations cosmic ν τ s ν τ identified by characteristic double shower events charged currect interaction + tau decay into hadrons and ν τ second shower has typically twice as much energy as first double bang

35 ν τ future speculations cosmic ν τ s shower size vs shower separation identified events will clearly result from vacuum neutrino oscillations, since without enhancement expect ν τ / ν µ < 10-5 ν τ events can be identified in under water/ice detectors

36 ν τ the ultra high energy neutrino universe OSCILLATIONS FLUXES OF ν τ AND ν µ ARE EQUAL neutrinos from interactions of ultrahigh energy cosmic rays with 3 K cosmic backgrond radiation neutrinos from AGNs, GRBs, etc Z bursts relic neutrinos from big bang cosmology

37 Conclusions direct observation of the tau neutrino by DONUT is an important milestone properties of tau neutrino like other neutrinos ν e, ν, ν µ, ν τ neutrino oscillations open up a variety of new future possibilities for ν τ in cosmology, astrophysics and future accelerators

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