Tau neutrino physics introduction
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Tau Neutrino Physics Introduction. Barry Barish 18 September 2000. n t – the third neutrino. The Number of Neutrinos big-bang nucleosynthesis. D, 3 He, 4 He and 7 Li primordial abundances. abundances range over nine orders of magnitude

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Tau neutrino physics introduction

Tau Neutrino PhysicsIntroduction

Barry Barish

18 September 2000


N t the third neutrino

nt – the third neutrino


The number of neutrinos big bang nucleosynthesis

The Number of Neutrinosbig-bang nucleosynthesis

D, 3He, 4He and 7Li primordial abundances

  • abundances range over nine orders of magnitude

  • Y < 0.25 from number of neutrons when nucleosynthesis began (Y is the 4He fraction)

  • Yobserved = 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.

  • YBBN= 0.012-0.014 N

1.7  N  4.3


The number of neutrinos collider experiments

The Number of Neutrinoscollider experiments

  • most precise measurements come from Z e + e

  • invisible partial width, 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

  • Standard Model value (  l)SM = 1.991  0.001 (using ratio reduces model dependence)

N = 2.984 0.008


Properties existence

 propertiesexistence

  • Existence was indirectly established from decay data combined with reaction data (Feldman 81).

  • DIRECT EVIDENCE WAS PRESENTED THIS SUMMER FROM FNAL DONUT EXPERIMENT

  • Observe thet and its decays from nt charged current interactions


Properties existence donut concept

 propertiesexistence – DONUT concept

  • calculated number of interactions = 1100 ( nm, ne, nt)

  • total protons on target = 3.6 1017

  • data taken from April to September 1997


Properties existence donut detectors

 propertiesexistence – DONUT detectors

Spectrometer

Emulsion-Vertex Detectors


Properties existence donut detectors1

 propertiesexistence – DONUT detectors

  • 6.6 106 triggers yield 203 candidate events


Properties existence donut events background

 propertiesexistence – DONUT events/background

4 events observed

4.1  1.4 expected

0.41± 0.15 background


Properties

 properties

J = ½

  • J = 3/2 ruled out by establishing that the is not in a pure H  -1 helicity state in 

magnetic moment

  • expect    for Majorana or chiral massless Dirac neutrinos

  • extending SU(2)xU(1) for massive neutrinos,

  • where m is in eV and B  eh/2me Bohr magnetons.

  • using upper bound mt < 18 MeV   < 0.6 10-11mB

  • Experimental Bound < 5.4 10-7mB from e  e (BEBC)


Properties1

 properties

electric dipole moment

< 5.2 10-17 e cm from (Z  ee) at LEP

nt charge

< 2 10-14 from Luminosity of Red Giants (Raffelt)

lifetime

> 2.8 1015 sec/eV Astrophysics (Bludman) for mn < 50 eV


N t properties direct mass measurements

ntpropertiesdirect mass measurements

  • direct bounds come from reconstruction of  multi-hadronic decays

  • LEP (Aleph)

  • from 2939 events   2 +  +< 22.3 MeV/c2

  • and 52 events  3 + 2 + () +  < 21.5 MeV/c2

  • combined limit< 18.2 MeV/c2


N t properties direct mass measurements1

nt propertiesdirect mass measurements

  • method

    • two body decay

    • t(Et,pt)  h (Eh,ph) + nt (En,pn)

    • tau rest frame – hadronic energy

    • Eh* = (mt2  mh2 +mn2) / 2mt

    • laboratory frame

    • Eh =  (Eh* +  ph* cos)

    • interval bounded for different mn

    • Ehmax,min = g (Eh*  b ph*)

two sample events

  3 + 2 + () + 


N t properties direct mass measurements2

nt propertiesdirect mass measurements

events & contours

0 MeV/c2 and 23 MeV/c2

Log-likelihood fit vs mn


N t properties direct mass measurements cosmological bounds

nt propertiesdirect mass measurements + cosmological bounds

Unstable nt

  • bounds on mnt from cosmology

  • combined with non observation of lepton number violating decay and direct mass limits


N t properties lepton sector mixing

nt propertieslepton sector mixing


N t properties oscillation probability

nt propertiesoscillation probability


N t properties oscillation phenomena

nt propertiesoscillation phenomena


N oscillations allowed regions

n oscillationsallowed regions


N oscillations atmospheric neutrinos

n oscillationsatmospheric neutrinos

Path length from ~20km to 12700 km


Atmospheric neutrinos ratio of n m events to n e events

atmospheric neutrinosratio of nm events to ne events

  • ratio-of-ratios (reduces systematics):

  • R = (nm/ne)obs / (nm/ne)pred

hint #1

ratio lower than expected


Atmospheric neutrinos angular distributions

atmospheric neutrinosangular distributions

Hint #2

anisotropy up/down and distortion of the angular distribution of the up-going events

Superkamiokande


Atmospheric neutrinos angular distributions with n oscillations

atmospheric neutrinosangular distributions with n oscillations


Atmospheric neutrinos energy dependence n oscillations

atmospheric neutrinosenergy dependence - n oscillations

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


N t properties mass difference neutrino oscillations

nt propertiesmass difference – neutrino oscillations

SuperKamiokande


Atmospheric neutrinos high energy events upward muons

atmospheric neutrinoshigh energy events – upward muons

MACRO Detector


Atmospheric neutrinos macro event types

atmospheric neutrinosMACRO event types

MACRO at Gran Sasso

  • Detector mass ~ 5.3 kton

  • Event Rate:

  • 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


Atmospheric neutrinos macro high energy events

atmospheric neutrinosMACRO high energy events

MACRO results


Atmospheric neutrinos macro evidence for oscillations

atmospheric neutrinosMACRO evidence for oscillations

Probabilities of nm nt 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 %


Atmospheric neutrinos agreement between measurements and experiments

atmospheric neutrinosagreement between measurements and experiments


Atmospheric neutrinos oscillation to sterile or tau neutrino

atmospheric neutrinososcillation to sterile or tau neutrino??

SuperKamiokande


Atmospheric neutrinos oscillation to sterile or tau neutrino1

atmospheric neutrinososcillation to sterile or tau neutrino??

MACRO

  • ratio (Lipari- Lusignoli, Phys Rev D57 1998) can be statistically more powerful than a c2 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.

  • nm nt oscillation favoured with large mixing angle:m2 ~ 2.5x10-3 eV2

  • sterile n disfavoured at ~ 2 slevel

test of oscillations

the ratio vertical / horizontal


Atmospheric neutrinos oscillation to sterile or tau neutrino2

atmospheric neutrinososcillation to sterile or tau neutrino??

SuperKamiokande

  • excluded regions using combined analysis of low energy and high energy data

  • Sobel n2000 stated ….


N t future speculations supernovae

ntfuture speculations - supernovae

SN1987a

What can be learned about the nt from the next supernovae ….??


N t future speculations supernovae1

ntfuture speculations - supernovae

  • direct eV scale measurements of m(nm) and m(nt) from Supernovae neutrinos

  • early black hole formation in collapse will truncate neutrino production giving a sharp cutoff

  • allows sensitivity to m(ne) ~1.8 eV for SN at 10 kpc in Superkamiokande detector

  • (Beacom et al hep-ph/0006015)

Events in SK

Low: 0 < E < 11.3 MeV

mid: 11.3 < E < 30 MeV

High: 30 < E < 


N t future speculations supernovae2

ntfuture speculations - supernovae

  • rate in OMNIS, a proposed supernovae detector

  • tail: 6.1 eV  2.3 events

OMNIS

delayed counts vs mass nt


N t the ultra high energy neutrino universe

ntthe ultra high energy neutrino universe

OWL - Airwatch

GZK cutoff – neutrinos ??


N t the ultra high energy neutrino universe1

ntthe ultra high energy neutrino universe

OSCILLATIONS

FLUXES OF nt AND nm

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


N t the ultra high energy neutrino universe2

ntthe ultra high energy neutrino universe


N t future speculations cosmic n t s

ntfuture speculations – cosmicnt’s

  • high energy n’s E > 106 GeV

  • neutrinos from proton acceleration in the cores of active galactic nuclei

  • vacuum flavor neutrino oscillationsenhance nt / nm ratio

  • detectable in under water / under ice detectors

  • (Athar et al hep-ph/0006123)


N t future speculations cosmic n t s1

ntfuture speculations – cosmicnt’s

  • ntidentified by characteristic double shower events

  • charged currect interaction + tau decay into hadrons and nt

  • second shower has typically twice as much energy as first

  • “double bang”


N t future speculations cosmic n t s2

ntfuture speculations – cosmicnt’s

  • shower size vs shower separation

  • identified events will clearly result from vacuum neutrino oscillations, since without enhancement expect nt / nm < 10-5

  • nt events can be identified in under water/ice detectors


Accelerators long baseline n m n t oscillations

Acceleratorslong baselinenm– nt oscillations

MINOS

K2K

CERN  GS


Accelerators long baseline n m n t oscillations1

Acceleratorslong baselinenm– nt oscillations

nt appearance


Accelerators neutrino factory neutrinos from muon collider

Acceleratorsneutrino factory – neutrinos from muon collider

muon collider

Example

7400 km baseline

Fermilab  Gran Sasso

“world project”

neutrino beams

select nm’s or anti nm’s


Accelerators neutrino factory neutrinos from muon collider1

Acceleratorsneutrino factory – neutrinos from muon collider

  • accurately determine n mixing matrix

  • perhaps even measure CP violation in n sector


Conclusions

Conclusions

  • direct observation of the tau neutrino by DONUT is an important milestone

  • properties of tau neutrino like other neutrinos ne, nm, nt

  • neutrino oscillations open up a variety of new future possibilities for nt in cosmology, astrophysics and future accelerators


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