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Neutrino Masses, Leptogenesis and Beyond The Incredible Foresight of ETTORE MAJORANA Haim Harari Erice, August 31, 2006
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Neutrino Masses, Leptogenesis and Beyond

Feb 25, 2016

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The Incredible Foresight of ETTORE MAJORANA Haim Harari Erice, August 31, 2006. Neutrino Masses, Leptogenesis and Beyond. b -Decay. e -. A 1  A 2 + e -. b -Decay. e -. e -. e -. e -. N 1  N 2 + e -. e -. e -. e -. e -. b -Decay. Missing Energy Missing Momentum . - PowerPoint PPT Presentation
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Page 1: Neutrino Masses, Leptogenesis and Beyond

Neutrino Masses, Leptogenesis and Beyond

The Incredible Foresight of ETTORE MAJORANA

Haim HarariErice, August 31, 2006

Page 2: Neutrino Masses, Leptogenesis and Beyond

A1 A2 + e-

e-

-Decay

Page 3: Neutrino Masses, Leptogenesis and Beyond

N1 N2 + e-

e-

e-

e-

e-

-Decay

Page 4: Neutrino Masses, Leptogenesis and Beyond

N1 N2 + e-

e-

e-

e-

e-

Missing EnergyMissing Momentum

-Decay

Page 5: Neutrino Masses, Leptogenesis and Beyond

N1 N2 + e- +

e-

e-

e-

e-

“Dear RadioactiveLadies & Gentlemen”

-Decay

Page 6: Neutrino Masses, Leptogenesis and Beyond

n p + e- +

np

np

e-

e-

e-

e-

e-

-Decay

Page 7: Neutrino Masses, Leptogenesis and Beyond

-Decay

d u + e- +

np

np

e-

e-

e-

e-

e-

e-

d

Page 8: Neutrino Masses, Leptogenesis and Beyond

The Elusive Neutrino

No Electric ChargeNo Strong InteractionsSpin = ½Only Weak InteractionsSmall or Zero Mass

1016

If 1016 reach earth - one will hit something somewhere.

With one thousand tons of water, and 1016 every second since the big bang - 1 EVENT !!! Pauli: “I have done

a terrible thing!”

Page 9: Neutrino Masses, Leptogenesis and Beyond

Creating Nuclei

n p + e- +

p n + e+ +

Creation of starsCreation of heavy elementsEnergy of the sunEnergy of starsExploding stars: supernova

The only way to convert a proton into a neutron

or vice versa – involves the neutrino!

n e- + p

p e+ + n

(Can you tell from ?)

Page 10: Neutrino Masses, Leptogenesis and Beyond

The SUN

4p He4 + 2e+ + 2 + Energy

Other Processes

Page 11: Neutrino Masses, Leptogenesis and Beyond

1957 - Neutrino Observed

Reines - Cowan

Big Problem: DETECTING Huge Problem: ELIMINATING BACKGROUND

Reactor n + p e+ + n

e+ + e- 2

n + Z Z’ +

Page 12: Neutrino Masses, Leptogenesis and Beyond

The Foresight

Can you tell a neutrino from an

anti-neutrino?

MAJORANA

may be its own antiparticle !

Page 13: Neutrino Masses, Leptogenesis and Beyond

Is Massless or Very Light ?

“Direct” experiments m (e) < few eV

TheoryNo good reason for massless Simple argument for very light . is the only “chargeless” particle.

All quarks and leptons “Dirac Mass” also “Majorana Mass”

Page 14: Neutrino Masses, Leptogenesis and Beyond

Is Massless or Very Light ?

m

“See-Saw”

M1 ~ O()M2 ~ O(m2/

0 mm

Majorana Mass

Gell-Mann, Ramond, Slansky, Yanagida

Page 15: Neutrino Masses, Leptogenesis and Beyond

Theorists predicted a new meson with a certain mass.

A particle was found soon after, having the right mass.

A second particle, very slightly heavier, was found soon after.

The second particle turned out to be the predicted meson.

The first particle turned out to be an unexplained heavy lepton,

identical to the electron in all its properties, except its mass.

Page 16: Neutrino Masses, Leptogenesis and Beyond

Theorists predicted a new meson with a certain mass.

A particle was found soon after, having the right mass.

A second particle, very slightly heavier, was found soon after.

The second particle turned out to be the predicted meson.

The first particle turned out to be an unexplained heavy lepton,

identical to the electron in all its properties, except its mass.

Yukawa ~100MeV

Anderson-Neddermeyer ~100MeV

Powell

m (e) = 0.51 MeV m () = 106 MeV

Page 17: Neutrino Masses, Leptogenesis and Beyond

Theorists predicted a new meson with a certain mass.

A particle was found soon after, having the right mass.

A second particle, very slightly heavier, was found soon after.

The second particle turned out to be the predicted meson.

The first particle turned out to be an unexplained heavy lepton,

identical to the electron in all its properties, except its mass.

m(e) = 0.51 MeV m() = 106 MeV

GIM D ~2000GeV

Perl ~1800MeV

SLAC-LBL

D

m() = 1782 MeV

Page 18: Neutrino Masses, Leptogenesis and Beyond

One or Two Neutrinos

eThe schizophrenic

pp

p

P

Detector

Brookhaven 1962

Is the “partner” of the same as the “usual” ,which comes with e ?

+ + +

Page 19: Neutrino Masses, Leptogenesis and Beyond

-6 -5 -4 -2-3 -1 -0 1 2 3 4 5 6 7 8 9 10 11 12eV meV eV MeVkeV GeV TeV

ud

ee

( )

( )

0

-1e

2/3

-1/3du

1stGeneration Q

e?Leptons

Quarks

Page 20: Neutrino Masses, Leptogenesis and Beyond

-6 -5 -4 -2-3 -1 -0 1 2 3 4 5 6 7 8 9 10 11 12eV meV eV MeVkeV GeV TeV

ud

ee

( )

( )

0

-1e

2/3

-1/3du

1stGeneration Q

sc

2nd

cs

( )

( )1970 GIM: “CHARM”

e? ?Leptons

Quarks

Page 21: Neutrino Masses, Leptogenesis and Beyond

-6 -5 -4 -2-3 -1 -0 1 2 3 4 5 6 7 8 9 10 11 12eV meV eV MeVkeV GeV TeV

ud

ee

( )

( )

e? 0

-1e

2/3

-1/3du

1stGeneration Q

sc

2nd

cs

( )

( )“The Standard Model”

tb

( )

( )

bt

3rd

Quarks

Leptons? ?

Page 22: Neutrino Masses, Leptogenesis and Beyond

ud( ) c

s( ) tb( )

“Mass Eigenstates”“Weak Eigenstates”

MixingMixingAngles(small)

Cabibbo

Page 23: Neutrino Masses, Leptogenesis and Beyond

Is Massless or Very Light ?

m

“See-Saw”

M1 ~ O()M2 ~ O(m2/

0 mm

Majorana Mass

Gell-Mann, Ramond, Slansky, Yanagida

Page 24: Neutrino Masses, Leptogenesis and Beyond

-12

-9

-6

-3

03

6

9

12

15

18

21

24

27

30

PeVTeV

GeVMeVkeVeV

meVeVneV

PlanckGUT

S.M.

tbc su de

e

Page 25: Neutrino Masses, Leptogenesis and Beyond

Pij = Sin 2 2ij Sin 2 (1.27 m2ij)

KmGeV

LE

· eV2

- Oscillations

An Identity CrisisReactor e

Accelerator

Sun e

e

Mass Eigenstates

GenerationEigenstates

APPEARANCEDISAPPEARANCE

Page 26: Neutrino Masses, Leptogenesis and Beyond

Three Mixing Angles

e 12 23

e 13

- Oscillations

Pij = Sin 2 2ij Sin 2 (1.27 m2ij)

KmGeV

LE

· eV2

LE m2 << 1 P ~ 0

m2 >> 1 P= ½ Sin2 2ijLE

m2 ~ O(1) probe mLE

Page 27: Neutrino Masses, Leptogenesis and Beyond

Reactors:

Accelerators:

E L Probe m2

MeV

GeV

m

km

eV>~eV>~

If mj >> mi m2ij ~ mj

2

All experiments were :e ee x x

- Oscillations

Hence: limits only on 12

Allowed Excluded

m2 eV2

1000

100

10

1

0.1

Sin2 2

Page 28: Neutrino Masses, Leptogenesis and Beyond

Cosmological Dark Matter

The universe is

95% is Dark matter or Dark EnergyWhat is the Dark Matter? Cosmic Background

Radiation: 2.7°Kper cm3: 400

110 e

110

110

If m(e ) + m() + m(~ O(few e)

ClosedOpenflat

Dark matter would be Hence: Crucial to search for

oscillations at O(eV)

Page 29: Neutrino Masses, Leptogenesis and Beyond

“CHORUS”CERN 1990 - 98

No events

cannot account for most of the dark matter in the universe!

Cosmological Dark Matter

Accelerator x