neutrinos: the big questions and how to answer them (and others)

Neutrinos: The Big Questions and How to Answer Them (and Others)

Manfred LindnerTechnical University Munich

„Future Perspectives in High Energy Physics“Kyungpook National University Sept. 28-Oct. 1, 2005, Daegu, Korea

Manfred Lindner The 8th ICFA Seminar 2

Motivation: Physics Beyond the SM

gauge hierarchy problemmH

2 ~ 2

SUSY ~TeV

3 generations, fermion rep.many parameters (mi ,mixings)unification into GUTs

m=(mD)TMR-1mD

~GUT

+seesaw

gauge bosons

Higgs

quarksleptons

experimental facts:Dark Matter & Dark Energyneutrino massesbaryon asymetry m> 0


New Physics: Neutrino Sources

Sun

Earth

Atmosphere

ReactorsCosmology

Accelerators

Astronomy: SupernovaeGRBsUHE ‘s


Parameters for 3 Light Neutrinos

mass & mixing parameters: m1 , m221, |m2

31| , sign(m231)

diag(eiei

normal invertedhierarchical or degenerate

questions: Dirac or Majorana absolute mass scale: m1

mass ordering: sgn(m231)

how small is 13, 23 maximal? leptonic CP violation LSND sterile neutrino(s) L/E pattern of oscillations

e


Four Methods of Mass Determination

• kinematical

• lepton number violation Majorana nature

• oscillations

• astrophysics & cosmology


Kinematical Mass Determination

Future: KATRIN 0.25 eV ? c.f. comological boundsKATRIN 0.25 eV


Heidelberg-Moscow experiment

< 0.35 eV ?

| |

free parameters: m1 , sign(m231) , CP-phases 2, 3

Neutrino-less Double -Decay

-

Majorana 02 decay


| m

ee|

in e

V

Lightest neutrino (m1) in eV

Phase II:

Phase III:

m1small mee =const. ~ (mij2)1/2 sign(m2

31)m1 large mee ~ m1

cosmological bound on m1

HM-claim ‚tension‘Phase I:

new experiments: CUORICINO, GERDACUORE, Majorana, …aim: (m31

2)1/2 ~ 0.05eV

Cosmology: syst. errors X10?02 nuclear matrix elements?theory: LR, RPV-SUSY, ...

lepton number violation

Feruglio Strumia Vissani


described by~ two independent

2x2 oscillationssurprise: large mixings!

Neutrino Oscillation Signals

m221 = (8.2+0.3) * 10-5 eV2

tan212 = 0.39 + 0.05m2

31 = (2.2+0.6) *10-3 eV2

tan223 = 1.0 + 0.3sin2213 < 0.16

solar

Reactors: KAMLAND

atmospheric

LSND? MiniBooNE

Beams: K2KMINOS


L/E Dependence: Atmospheric Oscillations

decoherence

decay

oscillation „dip"

oscillation

L/E dependence smeared out!


Result:• 3,4 for decay• 3,8 for de-coherence• m2=2.4 10-3eV2

long baseline exp.

Bad L/E resolution for:• horizontal events (dL/dcosis big!)• events with small energy

cuts in the E-cosplane

SK II datadecoherence decay oscillation


Testing Solar L/E with KamLAND

rate plus shape oscillations at 99.999995% CL

Best fit: m2=7.9+0.6-0.5×10-5eV2

tan2=0.46

improved tests of L/E:

• Super Kamiokande• KamLAND• MINOS• …


Solar Neutrinos: Learning About the Sun

Topics:- nuclear cross sections- solar dynamics - helio-seismology- variability- composition

Observables: - optical (total energy, surface dynamics, sun-spots, historical records, B, ...)- neutrinos (rates, spectrum, ...)


Learning from Atmospheric Neutrinos

primary cosmic-ray interaction in the atmosphere

cascade of secondaries,K

decay of secondaries

ee

neutrinos from decays of other particles

Issues (in flux models):- primaries (...)- atmosphere- cross sections- B-fields- shower models- ...


The Future of Oscillation Physics

long baseline experiments with neutrino beams reactor experiments with identical near & far detector

m2 and ij regions improved oscillation experiments controlled sources & detectors

Aims: improved precision of the leading 2x2 oscillations detection of generic 3-neutrino effects: 13, CP violation

=

S13 3 flavour effects S13

x Majorana-

CP-phases

matter effects

precision neutrino physics


New Neutrino Beams

• conventional beams, superbeams MINOS, CNGS, T2K, NOA, T2H,…

• -beams pure e and e beams from radioactive decays; ~ 100

• neutrino factories clean neutrino beams from decay of stored ’s

-

correlations & degeneracies


New Reactor Experiments

identical detectors many errors cancel

E=4MeV 2km 4km 40km 80km

no degeneraciesno correlationsno matter effects

Double Chooz KASKA Braidwood Angra, …


13 Sensitivity in the Next Generation

NOvA

T2K

Compare:• 5 years each • 5% flux uncertainty

next generation long baseline experiments

coming long baseline experiments

1 reactor +2 detectors

NOA

Huber, ML, Rolinec, Schwetz, Winter


Leptonic CP-Violationassume: sin2213= 0.1 , =/2 combine T2K+NOA+reactor

m2 > 0 m2 < 0 90%CL 3

bounds or measurements of leptonic CP-violation leptonic CP-violation in MR baryon asymetry via leptogenesis


Sensitivity Versus Time

-beamsneutrino factory

protondriver?


-Beam and / or NeutrinoFactory

• very powerful • interesting options• ...technological challenges

further R&D required

-beams: Store instable isotopes in accelerators pure e beams

-factory: Produce and store ‘s decay: pure e + beams_

neutrino factoryInternational

Scoping

Study


Incremental Path to a NeutrinoFactory

Era ofsensitivity &

precision

ISS: establish that afaster approach is possible

Era ofsensitivity &

precision


What is precison neutrino physicsgood for?

unique flavour information tests models / ideas about flavour history: elimination of SMA


The Value of Precision for 13

for example: sin2213 < 0.01

physics question: why is 13 so small ?

numerical coincidence symmetry

precision!

• models for masses & mixings• input: Known masses & mixings distribution of 13 „predictions“

• 13 often close to experimental bounds motivates new experiments 13 controls 3-flavour effects like leptonic CP-violation


Further Implications of Precision

Provides also measurements or tests of:

• MSW effect (coherent forward scattering and matter profiles)• cross sections• 3 neutrino unitarity sterile neutrinos with small mixings• neutrino decay (admixture…)• decoherence• NSI• MVN, ...

• special angles: 13= 0°, 23= 45°, ... discrete f. symmetries?• special relations: 12+ C = 45° ? quark-lepton relation?• quantum corrections renormalization group evolution

Precision allows to identify / exclude:


The Interplay of Topics

mass spectrum, mixings, CP-phases, LVF, 02decay, ...

SM extensions

flavour symmetries Leptogenesis,supernovae, BBN,structure formation,UHE neutrinos, ...

renormalization group

-parameters extremely valuable long term: most precise flavour info

neutrino properties:masses, mixings,

CP-phases, ...


Neutrinos & Cosmology

• Dark Matter ~ 25% & Dark Energy 70% • mass of all neutrinos: 0.001 < < 0.02• baryonic matter ~ 0.04

neutrinos affect:

- BBN, structure formation

- baryon asymmetry, ...


Cosmology and Neutrino Mass• ‘s are hot dark matter smears structure formation on small scales

•WMAP+2dFGRS + Lymass bound: m< 0.7 ... 1.2 eV• degenerate neutrinos m < 0.4 eV future improvements: ~factor 5-10 ?• comparison with 02, LSND • will be directly tested by KATRIN

f=/matter

Tegmark


Baryon Asymmetry & Neutrinos

anti-mattermatterparticle anti-particle

symmetry

baryon-

asymmetry

theory observation

measured baryon asymmetry:

Necessary: Sakharov conditions:• B-violating processes sphalerons• C- and CP-violation contained in model • departure from thermal equilibrium < H

natural explanation of baryon asymmetry by leptogenesis

• minimal leptogenesis works nicely• different interesting variants ... a talk by itself


• Collaps of a typical star ~1057 ‘s• ~99% of the energy in ‘s• ‘s essential for explosion • 3d simulations do not explode (so far... 2d3d, convection? ... )

Supernova Neutrinos

MSW: SN & Earth

Very sensitive to finite 13 and sgn(m2)

Dighe, Smirnov


2 possibilities:

Supernova

neutron star or black hole

Keeps cooling... abrupt end of emission

• impressive signal of a black hole in neutrino light • neutrino masses edge of -signal


Supernovae & Gravitational Waves

gravitational wave emission quadrupol moment of the explosion

additional information about galactic SN global fits: optical + neutrinos + gravitational waves neutrino properties + SN explosion dynamics SN1987A: strongest constraints on large extra dimensions

Dimmelmeier, Font, Müller


Neutrinos from Glactic Center

galactic

center

p n

+ 0 ´s

HE ´s @ HESS, EGRET

SN shock front acceleration flux from GC signal @ km3 detectors

HESS: TeV ‘s


Geo Neutrinos as Probes of the Earth

Neutrino flowNeutrino flow

Heat flowHeat flow

- radiogenic part of terrestrial heat flow ~80 mW/m2 total: ~40 TW - test geochemical model of the Earth, the BBulk SSilicate EEarth- test unorthodox ideas of Earth’s interior (K @ core, giant reactor)


Geo-Neutrino Observation at KamLAND

U+Th geo- candidates: 25+19-18

BSE model expectation: 19 Observed e candidates 152 eventsExpected total backgrounds 127±13

Reactor 13C(,n)16O

238U232Th

Accidental

Expected total backgrounds

Expected total

2nd reactor results

Geo-


Conclusions

Neutrinos probe new physics in many ways!


New Ideas: LENAIdea: ~30 kt underground liquid scintillator detector neutrino properties (solar, atmospheric, reactor, beams) solar neutrino spectroscopy supernova relic neutrino detection galactic supernova burst detection geo neutrino detection proton decay p K+ (favoured in SUSY models) - K invisible in water - better energy resolution - K and decay producs observable in scintillator - t > 3 * 1034y

K

nsecscintillator good resolution

water~SKbad resolution

modulation


combined

New Ideas: R2D2 - Reactor Experiments• Symmetric reactors,detectors:

– R1, R2, D1, D2 - may be different

– L11=L22 and L12=L21

• Separate events from R1 and R2

– R1 and R2 on/off times

– Neutron displacement

• Simplest case: 1d line-upHigh statistics: precise statistical separation

N11, N21, N12, N22 self-calibration:

N11/N21=N22/N12

oscillation

stable against size, backgrounds, ... Improved sensitivity

Rr

NN

NN4

4

12*21

22*11

1,5cm

6cm

R1

at detector D1:

R2


13 in the Coming LBL Generation

neutrinos: the big questions and how to answer them (and others)

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