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Leptogenesis and Neutrino Physics. 2011.4.7 연세대학교 강신규 ( 서울과학기술대 ). Outline. Introduction - baryogenesis Baryogenesis in some models Leptogenesis Informations on neutrino masses from leptogenesis Neutrinoless double beta decay

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leptogenesis and neutrino physics

Leptogenesis and Neutrino Physics

2011.4.7

연세대학교

강신규(서울과학기술대)

outline
Outline
  • Introduction

- baryogenesis

  • Baryogenesis in some models
  • Leptogenesis
  • Informations on neutrino masses from leptogenesis
  • Neutrinoless double beta decay
  • Connection between leptogenesis and neutrinoless double beta decay
  • Summary
slide3
Introduction
  • Inflation explains r=rcr
  • Big-bang explains ne=np, n4He/np=0.125,
  • nD/np=1.5x10-5, nn/ng=3/22 , etc.
  • We do not understand nB/ng
slide4
Measuring nB/ng= 6 · 10−10
  • - Tnow ~ 3K directly tells ng~ T3now ~ 400/cm3.
  • - nB ~ 1/m3 follows from
  • Anisotropies in the cosmic microwave background:
  • nB/ng= (6.3±0.3)x10−10.

(2) Big Bang Nucleosynthesis: the D abundancy implies

nB/ng= (6.1±0.5)x10−10.

arisen from many g push in the direction reactions like

p n D g

(1) and (2) are indirect but different: their agreement makes the result trustable.

slide5
nB/ng= 6 · 10−10 is a strange number, because means that when the universe cooled below T ~ mp , we survived to nucleon/antinucleon annihilations as

10,000,000,001 nucleons

10,000,000,000 anti-nucleons

Nucleons and anti-nucleons got together…

slide6
They have all annihilated away except for the tiny
  • difference.

1 nucleon

  • That created tiny excess of matter in the present
  • universe (unnatural !!!)

nB/ng = 6 · 10−10

slide7
Can a asymmetry can be generated dynamically from nothing?

Yes, if 3 Sakharov conditions are satisfied

  • Necessary requirements for baryogenesis:
    • Baryon number violation :
    • C & CP violation :
    • Non-equilibrium
slide8
Out-of-Equilibrium Decay

Out-of Equilibrium obtained due to expansion of the Universe as a background for heavy decaying particles.

Condition for out-of-equilibrium decay

slide9
Boltzmann Equation

If interactions becomes too slow to catch up with expanding Universe, NX start to become overabundant.

We must consider inverse decays, scatterings and annihilations

RHS  NXvariation due to all elementary processes for X

slide11
Coupled Equations for nX and nB-L

CP asymmetry

washout at T

In the SM not all of the dynamics is described by perturbative effects; There are non-perturbative interactions that violate B+L.

slide12
Sphaleron

Non-perturbative finite temperature interactions, involving all left chiral fermions (due to chiral nature of weak interactions)

Above EW-scale sphaleron processes (violating B+L) are in equilibrium and conserve B-L.

Below EW-scale Higgs vev suppresses sphaleron rates

 constrains models of EW Baryogenesis.

slide13
Baryogenesis in the standard model
  • Sakharov’s conditions
    • B violation EW anomaly (Sphaleron)
    • CP violation KM phase
    • Non-equilibrium 1st order phase trans.
    • Standard Model may satisfy all 3 conditions!
  • Electroweak Baryogenesis(Kuzmin, Rubakov, Shaposhnikov)
  • Two big problems in the Standard Model
    • 1st order phase transition requires mH < 60GeV
    • CP violation too small because
    • J  det[Yu†Yu, Yd†Yd]~ 10–20<< 10–10
slide14
Original GUT Baryogenesis
  • GUT necessarily breaks B.
  • (there exist several B violating interactions)
  • A GUT-scale particle X decays out-of-equilibrium with direct CP violation
  • But keeps B–L0  “anomaly washout”
  • Monopole problem
  • Alternative scenarios required (B-L violation)
slide15
Leptogenesis:

role of neutrinos in baryogenesis

slide16
Seesaw MechanismPrerequisite for Leptogenesis
  • Why is neutrino mass so small?
  • Need right-handed neutrinos to generate tiny neutrino mass, but nR SM neutral
  • Majorana neutrinos: violate lepton number (B-L violation)

To obtain m3~(Dm2atm)1/2, mD~mt, M3~1015GeV

(GUT!)

slide17
(SM)

Basic Leptogenesis Mechanism

  • Fukugita and Yanagida ’86
  • Based on standard out-of-equilibrium decay of a heavy particle:
  • 1. CP violating decay of a heavy particle through an L-violating interaction can produce a lepton asymmetry.
  • 2. This lepton asymmetry is transformed into a
  • baryon asymmetry through sphaleroninteractions :
slide18
CP Asymmetry
  • CP violation through phases in neutrino sector.
  • CP asymmetry produced through interference of tree and one-loop contribution of decay rate.
slide19
abundance at eq.
  • Decay rate :
  • Lepton number asymmetry
  • e : CP asymmetry determined by the particle physics model that
  • produces couplings and masses for NR
  • k (efficiency) : incorporates washout effects by L-violating interactions
  • after the RH neutrinos decay.
slide20
Baryon asymmetry determined by 4 parameters
  • CP asymmetry e1
  • Mass of decaying neutrino M1
  • Effective light neutrino mass (coupling strength of N1)
  • Light neutrino masses
slide23
Some constraints from Leptogenesis

(1) Heavy neutrino mass

 depends on the NR mass hierarchy

(i) Very hierarchical

Assuming

  • When vertex diagram becomes dominant
  • (Davidson & Ibarra)
slide25
(ii) hierarchical M2,3~10-100M1

small

can be large

For example) are

compatible with successful leptogenesis with special

Yukawa matrix

slide26
(iii) Quasi-degenerate case M1~M2

Huge resonance peak if

  • No more mn constraints on leptogenesis
  • No more lower limit on heavy Majorana mass
  •  TeV scale leptogenesis possible
  •  Resonant leptogenesis
slide27
(2) Light neutrino masses
  • mnconstraints on the size of e
slide28
Refinement by Buchmuller et al. for constraint on ε

Considering the efficiency k which depends on

slide29
Thermal leptogenesis fails if ns are too heavy and degenerate due to:

the domain shirnks to zero

yields

upper limits on mi

slide30
Nodependence on intial

abundance of N1 for

slide31
Since , leptogenesis window for neutrino mass

compatible with neutrino oscillation

can we prove it experimentally
Can we prove it experimentally?
  • Unfortunately, no: it is difficult to reconstruct relevant CP-violating phases from neutrino data
  • But: we will probably believe it if
    • 0nbband/or LNV processesfound
    • CP violation found in neutrino oscillation
    • EW baryogenesis ruled out
cp violation
CP Violation
  • Possible only if:
    • Dm122, s12 large enough (LMA)
    • q13 large enough
  • Can we see CP violation?

 KamLAND

 Reactor Exp. ?

 ?

It may need better parameter determination using solar pp neutrinos

slide35
With the discovery that neutrinos are not massless, there is intense interest in neutrinoless double-beta decay (0nbb) measurements.
  • 0nbb decay probes fundamental questions :
  • Lepton number violation : leptogenesis might be the
  • explanantion for the observed matter-antimatter
  • asymmetry.
  • Neutrino properties : the practical technique to
  • determine if neutrinos are their own anti-particle :
  • Majorana particles.
if 0 nbb decay observed
If 0nbb decay observed :
  • Violates lepton number :
  • Neutrino is a Majorana particle.
  • Provides a promising lab. method for determining the absolute neutrino mass scale that is complementary to other measurement techniques
  • Measurements in a series of different isotopes potentially can reveal the underlying interaction processes.
  • Establishing that neutrinos are Majorana particles would be as important as the discovery of neutrino oscillations
neutrinoless double beta decay
Neutrinoless double beta decay

Lepton number violation

Baryon asymmetry  Leptogenesis due to

violation of B-L number

slide38
The half-life time, , of the 0nbbdecay can be factorized as :

: phase space factor

: Nuclear matrix element

:depends on neutrino mass hierarchy

best present bound
Best present bound :

Heidel-Moscow

Half-life

Consistent with cosmological bound

slide41
If neutrinos are Majorana particles
  • Neutrino oscillations :

- not sensitive to the nature of neutrinos

- provide information on , but not on

the absolute values of neutrino masses.

slide42
Neutrino mass scale and its property can be probed
  • by 0nbb
  • Prediction of depends on neutrino mass hierarchy
slide43
Normal hierarchy:
  • Inverted hierarchy
slide44
Quasi-degenerate
  • Estimate by using the best fit values of parameters including uncertainties in Majorana phases
slide45
( Hirsch et al. , hep-ph/0609146 )

For inverted hierarchy, a lower limit on obtained

8 meV

slide46
In principle, a measurement of || combined with a measurement of m1(mass scale)
  • (in tritium beta-decay exp. and/or cosmology)
  • would allow to establish if CP is violated.
  • To constrain the CPV phases,
  • once the neutrino mass spectrum is known
slide47
Due to the experimental errors on the parameters and nuclear matrix elements uncertainties, determining that CP is violated in the lepton sector due to Majorana CPV phases is challenging.
  • Given the predicted values of , it might be possible only for IH or QD sepctra. In these two cases, the CPV region is inversely proportional to
  • Establishing CPV due to Majorana CP phases requires
  • Small experimental errors on and neutrino masses
  • Small values of
  • depends on the CPV phases :
connection between low energy cpv and leptogenesis
Connection between low energy CPV and leptogenesis
  • High energy parameters Low energy parameters
  • 9 parameters are lost, of which 3 phases.
  • In a model-independent way there is no direct connection between the low-energy phases and the ones entering leptogenesis.
slide49
Using the biunitary parameterization,
  • depends only on the mixing in RH sector.
  • mndepends on all the parameters in Yn .
  • If there is CPV in VR, we can expect to have CPV in mn.
  • In models witha reduced number of model parameters,
  • it is possible to link directly the Dirac and Majorana phases to the leptogenesis one.
  • Additional information can be obtained in LFV charged lepton decays which depend on VL.
slide50
Existence of a correlation

between

  • In minimal seesaw with two heavy Majorana neutrinos
  • (Glashow, Frampton, Yanagida,02)
  •  mDcontains 3 phases

(Endo,Kaneko,SK,Morozumi,Tanimoto)

(2002)

slide52
Type II Seesaw (for MR1 << MR2, MR3 , MD ) (S.F.King 04)

Bound on lepton asymmetry

for neutrino mass scale

(in sharp contrast to type I)

For successful thermal leptogenesis :

MR1for neutrino mass scale

Bound on type II MR 1lower than Type I bound

summary
Summary
  • Although current precision observation on baryon asymmetry in the universe, we do not know how it can be dynamically generated.
  • Leptogenesis is a plausible mechanism for baryogenesis.
  • Since neutrinos play an important role in leptogenesis,

we can obtain some informations on neutrino masses

requiring for successful leptogenesis

  • Neutrinoless double beta decay can probe neutrino property and mass hiererchy and CP violation, which are

closed related with leptogenesis.

slide54
Constraints on leptogenesis
  • Type I Seesaw (for MR1 << MR2, MR3) (S. Davidson et al. 02)

Bound on lepton asymmetry

for neutrino mass scale

For successful thermal leptogenesis :

MR1for neutrino mass scale

Lower bound on MR1 :

ad