neutrinos as probes of new physics manfred lindner technical university munich susy05 the 13th...

Neutrinos as Probes of New Physics

Manfred LindnerTechnical University Munich

SUSY05The 13th International Conference on Supersymmetry and Unification of Fundamental Interactions July 18-23, 2005, IPPP Durham, UK

Manfred Lindner SUSY05 2

New Physics: Beyond the Standard Model

Two directions beyond SM:• EW symmetry breaking & hierarchy problem Higgs, SUSY, ... LHC, LC, ...• flavour problem origin of generations, flavour symmetries, q-l relations, .... neutrino physics, ...

Experimental facts• Cold Dark Matter & Dark Energy exist!• neutrino masses have been detected!• baryon asymetry of the universe m> 0

physics beyond the standard model


New Physics: Neutrino Sources

Sun

Earth

Atmosphere

ReactorsCosmology

Accelerators

Astronomy: SupernovaeGRBsUHE ‘s


Parameters for 3 light Neutrinos

diag(eiei

diag(eiei

4 different methods:

• kinematical

• lepton number violation Majorana

• oscillations

• astrophysics & cosmology


Kinematical Mass Determination


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 ~ (mij2)1/2

sign(m231)>0 ij=12

m1 large mee ~ m1

cosmological bound on m1

HM-claim ‚tension‘Phase I:

new exp. e.g. GERDAaim: (m31

2)1/2 ~ 0.05eV

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

lepton number violation

Feruglio Strumia Vissani


Neutrino Oscillation Signals

m2

21= 7.9 10-5 eV2

sin212 = 0.314m2

31= 2.4 10-3 eV2

sin223 = 0.44

solar

Reactors (KAMLAND)

atmospheric

LSND? MiniBooNE

Beams (K2K)


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- X-sections- B-fields- shower models- ...


The Future of Neutrino Oscillations

„long baseline“ experiments with neutrino beams and reactors

1) Improved precision of the leading 2x2 oscillations 2) Detection of generic 3-neutrino effects 13, CP-phase sgnm2

precision neutrino physics

3 flavour-oscillations

+ matter effects sgnm2

=

S13 3f-effects S13

x Majorana-

CP-phases


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


Long Term Ideas: -Beam & -Factory

• very powerful• interesting options• many good ideas• ...technological challenges

further R&D required

-beam idea: Store instable isotopes in accelerators pure e beams

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

_


What is precison neutrino physicsgood for?

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


13: What to expect from Flavour Models

For example: Ue3 in models with U(1) flavour symmetry Altarelli, Masina

[SS] [SS]

[SS] [NoSS]

Ue3 peaks close

to Chooz bound

sin2213<0.02 would select a very narrow subset of models

0.02 < sin2213 would not favour a particular model or spectrum

``anarchy’’= random numbers also favours 13 close to bounds

de Gouvêa, Murayama


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 CP-violation


Further Implications of Precision

Provides also tests of:

• MSW effect (coherent forward scattering and matter profiles)• 3 neutrino unitarity sterile neutrinos with small mixings• neutrino decay• 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:


Mass Models & Renormalization

low energies:• small masses• large mixings

high energies:• mass models• flavour-symmetries• GUT-models, ...

renormalization group running

atmospheric

solar

reactor

bi-maximal

Small or even zero

MSSM example:Antusch, Kersten, ML, Ratz

23=

13 versus limit/value


Neutrino Mass Operators

d=4 renormalizable mass operatorsnatural scale symmetry

xL

xL

SM with L only m=0 introduce R = 1L

xx

L R

<> = v

R RgN

Majorana, L/

R

L

RD

DRL Mm

m

0

seesaw mechanism (type I)

m=mDMR-1mD

T mh=MR

For m3 ~ (m2atm)1/2, mD ~ leptons MR ~ 1011 - 1016GeV

neutrinos are Majorana particles , m probes ~ GUT scale physics! smallness of neutrino masses high scale of L, symmetries of mD , MR

/


More Mass Operators

xL L

<L>ML = 0 / m=ML - mDMR

-1mDT

Seesaw type II

More general:• mass matrix for all neutrino-like fields• every term has a natural scale symmetries GUT, flavour symmetry, lepton number, ...• diagonalization complicated dependence on all parameters

mechanisms to produced large mixings: e.g. sequential dominance King, ...


Screening

fit fermions into GUT representations relation between Yukawa couplings, e.g. E6

Assume: L, CR, S

double seesaw

complete screening of Dirac structure

m Planck scale symmetries, QLC, ... ML, Schmidt Smirnov


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

GC

p n

+ 0 ´s

HE ´s @ HESS, EGRET

flux from GC signal @ km3 detectors

HESS: TeV ‘s


• X-sections• NuTEV-anomaly• GRBs• AGNs• horizontal air showers @ Auger• regenerationOWL, ...• ...• theory: - models of -masses & mixings & RGE effects - scenarios with N>3 (sterile ‘s + small mixings) - limits on neutrino decay - bounds for non-standard interactions - big bang nucleosynthesis - conncetions to >SM & electro-weak symmetry breaking - GUTs, discrete flavour-symmetries - extra dimensions, strings, ... - ...

Other Topics (not covered)


Conclusions

Neutrinos probe new physics in many ways!

neutrinos as probes of new physics manfred lindner technical university munich susy05 the 13th...

Documents

neutrino masses

flavour effects

flavour symmetries

neutrino effects q13

neutrino beams

flavour history

flux models

flavour modelsfor example