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Seesaw 25. Paris, 10-11/06/04. P. Binétruy, APC, Paris. SEESAW 25 The program. Thursday June 10th Morning Session Chairman P. Frampton (Univ. of North Carolina) 09:30 Welcome P. Binétruy (LPT, Orsay & APC, Paris)

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Seesaw 25

Seesaw 25

Paris, 10-11/06/04

P. Binétruy, APC, Paris


SEESAW 25 The program

Thursday June 10th

Morning Session Chairman P. Frampton (Univ. of North Carolina)

09:30 Welcome P. Binétruy (LPT, Orsay & APC, Paris)

09:40 Seesaw and the riddle of massP. Ramond (Gainesville)

10:20 LeptogenesisT. Yanagida (Tokyo)

11:00 Coffee break

11:30 Various realizations of the seesaw mechanismR.N. Mohapatra (Maryland)

12:00 Seesaw mechanism and GUTsG. Senjanovic (Trieste)

Afternoon Session (1) Chairman S. Bilenky (SISSA, Trieste)

14:30 The experimental evidence for neutrino massK. Heeger (Berkeley)

15:10 Textures and flavour modelsG.G. Ross (Oxford)

15:40 Seesaw mechanism and renormalization group effectsM. Lindner (Munich)

16:10 Coffee break

Afternoon Session (2) Chairman E. Ma (Univ. of California, Riverside)

16:40 Seesaw mechanism and supersymmetryA. Masiero (Padua)

17:10 CP violation in the seesaw mechanismJ. Hisano (Tokyo)


Friday June 11th

Morning Session (1) Chairman R. Hahn (Brookhaven Nat. Lab.)

09:00 13and CP violation in the lepton sectorC. Hagner (Hamburg)

09:30 Seesaw mechanism and the baryon asymmetryM. Raidal (Tallinn)

10:00 Various realizations of leptogenesis and neutrino mass constraints

Th. Hambye (Oxford)

10:30 Coffee break

Morning Session (2) Chairman G. Raffelt (MPI, Munich)

11:00 Seesaw mechanism and extra dimensionsE. Dudas (Orsay)

11:30 Neutrinos and astrophysicsS. Hannestad (Odense)

12:00 Detectors for low-energy neutrinos and CDMS. Schoenert (Heidelberg)

Afternoon Session Chairman C. Albright (Fermilab)

14:00 Seesaw mechanism beyond neutrino physicsT. Appelquist (Yale)

14:30 Alternatives to the seesaw mechanism A. Yu. Smirnov (Trieste)

15:00 Searching for the absolute neutrino mass scale Ch. Weinheimer (Bonn)

15:30 Can one reconstruct the seesaw parameters? S. Davidson (Durham)

16:00 Coffee break

16:30 Round table Moderator J. Orloff (LPC, Clermont-Ferrand)

« How to probe the origin of neutrino masses? »

G. Gratta (Stanford) - B. Kayser (Fermilab) - S. Raby (Columbus) -

J.W.F. Valle (Valencia) - Ch. Wetterich (Heidelberg)


The seesaw mechanism places the neutrino center stage :

Lepton

Flavour

violations

SUSY

Extra

dimensions

Masiero

Gravitino

problem

Dudas

Inflation

M =mLT MR-1 mL

Yanagida

Left-Right

symmetry

Mohapatra

Leptogenesis

GUT

Hambye, Raidal, Lindner

Flavor

symmetries

Senjanovic, Lindner

Ramond, Ross


The seesaw mechanism places the neutrino center stage :

M =mLT MR-1 mL

Left-Right

symmetry

Mohapatra

GUT

Flavor

symmetries

Senjanovic, Lindner

Ramond,Ross


Mohapatra

seesawthors



Mohapatra

GUTS

LR


Lindner

Importance of renormalization group effects



Need to identify the absolute

mass scale !

Ramond


THE ABSOLUTE VALUES OF NEUTRINO MASSES

FROM COSMOLOGY

NEUTRINOS AFFECT STRUCTURE FORMATION

BECAUSE THEY ARE A SOURCE OF DARK MATTER

NEUTRINOS AFFECT STRUCTURE FORMATION

BECAUSE THEY ARE A SOURCE OF DARK MATTER

HOWEVER, eV NEUTRINOS ARE DIFFERENT FROM CDM

BECAUSE THEY FREE STREAM

SCALES SMALLER THAN dFS DAMPED AWAY, LEADS TO

SUPPRESSION OF POWER ON SMALL SCALES

S. Hannestad


mn = 0 eV

mn = 1 eV

mn = 0 eV

Ma ’96

mn = 7 eV

mn = 4 eV


BEST FIT TO DATA IS NOT AT mn = 0, EVEN IF NO

INFORMATION ON BIAS IS USED

HOWEVER, mn = 0 IS NOT EXCLUDED EVEN AT 2s

THE PRESENT UPPER BOUND ON NEUTRINO MASS

IS

Warning : THERE COULD BE MORE THAN ONE

NON-STANDARD EFFECT, SEVERELY BIASING

THE PARAMETER ESTIMATE

S. Hannestad




Ross :

Ramond


The seesaw mechanism places the neutrino center stage :

SUSY

Gravitino

problem

Inflation

M =mLT MR-1 mL

Yanagida

Leptogenesis

Hambye, Raidal, Lindner




But gravitinos are produced by thermal scattering processes after inflation

TR < 104-5 GeV

for m3/2 ~ TeV

Yanagida favors light gravitino:

100 keV < m3/2 < 10 GeV


The seesaw mechanism places the neutrino center stage : after inflation

Lepton

Flavour

violations

SUSY

Extra

dimensions

Masiero

Dudas

M =mLT MR-1 mL


Masiero after inflation

BLABL

A


Masiero after inflation


Typology of seesaw after inflation

or

Seesaw or not seesaw?

Type I

Type II or induced triplet?

Magg, Wetterich ‘80

Hambye


Can one test the seesaw idea? after inflation

NO !

  • One cannot test a mechanism.

  • One can only test a theory, i.e. the realization of this mechanism in an explicit theory


More doubts if after inflation

light sterile neutrinos are found (LSND/MiniBOONE)

neutrino mass spectrum turns out to be quasi-degenerate

Again, both these features

can be accommodated in seesaw:

Seesaw + additional symmetry ->

three active + 1 sterile neutrino

R.Mohapatra

- Seesaw I + symmetry (e.g., SO(3))

- seesaw II + symmetry

- ``cascade seesaw’’:

S.Petcov, A.S.

E.Ma

J. Valle

0 mD 0

mn = mD 0 MD

0 MD M

If MD = A mD,

and M = M0I

mn ~ M0 /A2 I

A Yu Smirnov


2. No way to prove? after inflation

Will not prove that seesaw

is the main mechamism

Discovery of the neutrinoless

double beta decay

Leptogenesis

Difficult to test also

In SUSY context:

lepton violating decays,

EDM, ...

Indirect,

assumptions...

Easy to disprove seesaw as

the dominant mechanism of

neutrino mass generation

A Yu Smirnov


Roundtable : C. Wetterich after inflation

  • Induced triplet (type II seesaw) mechanism dominates if :

  • maximal - mixing from generation symmetry (1 - sin2  < 0.01)

  • degenerate neutrino masses

Heated debate around these statements….



Thanks to the local organizing committee, after inflation

in particular S. Lavignac, J. Dumarchez and I. Cossin