Xing Zh., Zhou Sh. Neutrinos in Particle Physics, Astronomy and Cosmology

416 11 Cosmological Matter-antimatter Asymmetr

y

i

nEq.

(

11.74

)

. After the summation over all the processes involving the ta

u

l

eptons, the interaction rate is

g

iven b

y

Γ

τ

ΓΓ

≡

γ

τ

n

eq



≈

10

−

3

y

2

τ

T.

(

11.115

)

C

omparin

g

Γ

τ

ΓΓ

with the Hubble

p

aramete

r

H

≈

1

.

66

√

g

√√

∗

T

2

/M

pl

MM

,

one

ﬁ

nd

s

that

Γ

τ

ΓΓ

>H

holds whe

n

T<

10

1

2

G

eV. In a similar wa

y

one ma

yﬁ

nd tha

t

the Yukawa interactions of the muon le

p

tonscanbeinthermale

q

uilibrium

a

r

ou

n

d

T

∼

10

9

G

eV. When the temperature drops below

T

∼

10

5

G

eV, al

l

the char

g

ed-lepton Yukawa interactions are

f

aster than the expansion rate o

f

the Universe

(

Barbier

i

et al.

,

2000

;

Endoh et al., 2004; Vives, 2006

)

.

I

nt

h

e temperature ran

g

e10

12

G

e

V

>T >

10

9

G

eV, the tau

ﬂ

avo

r

i

sdistin

g

uishable but the electron and muon

ﬂ

avors are indistin

g

uishable.

A

s a consequence, the tau-ﬂavor component of the lepton stat

e

|



i



fro

m

the

N

i

N

d

ecays s

h

ou

ld b

esin

gl

e

d

out an

d

t

h

en t

h

e inverse

d

ecays may ta

ke

p

lace as 

τ

+

H

→

N

i

NN

a

n

d



o

+

H

→

N

i

NN

,

wher

e

|



o



d

enotes the non-tau

ﬂavor component orthogonal t

o

|



τ



. Both the CP-violating asymmetry and

washout e

ﬀ

ects associated with the tau

ﬂ

avor should be treated separatel

y,

s

o it is necessar

y

to have two Boltzmann equations for the lepton numbe

r

a

s

y

mmetr

i

e

s

Y

(

τ

)

L

YY

a

nd

Y

(

o

)

L

Y

. To see the ﬂavor eﬀects in a clear wa

y

, we consider

the

N

1

NN

-dominated leptogensis in the full ﬂavor regime with T



10

9

G

e

V

and

a

ll the lepton

ﬂ

avors bein

g

distin

g

uishable. First, the

ﬂ

avor-dependent

C

P-

violating asymmetries

ε

1

α

(

fo

r

α

=

e, μ,

τ

)

should be calculated. A particula

r

c

ase is that the success

f

ul lepto

g

enesis mi

g

ht be achieved

f

ro

m

ε

1

α



= 0 even



thou

g

h the total

C

P-violatin

g

asymmetry

ε

1

is vanishin

g

or vanishin

g

ly smal

l

(

i.e.

,

ε

1

=

ε

1

e

+

ε

1

μ

+

ε

1

τ

≈

0) (

Nardi

e

tal

.

,

2006

;

Abada et al., 2006

)

. Second

,

the e

ﬃ

ciency

f

actor

s

κ

1

α

can be computed via the e

ﬀ

ective neutrino masses

˜

m

1

α

≡

|

(

Y

ν

YY

)

α

1

|

2

(

Y

†

ν

YY

Y

ν

Y

)

11

˜

m

1

.

(

11.116

)

The values of ˜

m

1

α

characterize the washout eﬀects of diﬀerent ﬂavors. Finally,

t

h

esp

h

a

l

eron processes conserve t

h

e quantum num

b

er

Δ

α

=

B/

3

−

L

α

,as

i

ndicated below Eq.

(

11.13

)

. In the temperature range under consideration,

t

h

e processes in t

h

erma

l

an

d

c

h

emica

l

equi

l

i

b

rium inc

l

u

d

ea

ll

t

h

e gauge in

-

teractions, strong and electroweak sphaleron interactions,

(

t,

b

,

c

)

-quark and

(

τ

,

μ

)

-lepton Yukawa interactions. After imposing the hypercharge conserva

-

tion and the equilibrium conditions of chemical potentials, one can obtain

(

Abad

a

et al

., 2006; Nar

di

et al.

,

2006; Davi

d

so

n

et al.

, 2008

)

⎛

⎜

⎛

⎝

⎜⎜

Y

L

YY

e

Y

L

YY

μ

Y

L

YY

τ

⎞

⎟

⎞⎞

⎠

⎟⎟

=

⎛

⎝

⎛⎛

−

151

/

179

2

0

/

179

2

0

/

1

79

25

/

358

−

3

44

/

537 1

4

/

53

7

25

/

358 1

4

/

5

3

7

−

3

44

/

53

7

⎞

⎠

⎞⎞

⎛

⎜

⎛⎛

⎝

⎜⎜

Y

Δ

Y

e

Y

Δ

Y

μ

Y

Δ

Y

τ

⎞

⎟

⎞⎞

⎠

⎟⎟

.

(

11.117

)

This result, to

g

ether with

Y

B

Y

=2

8

/

79

×

(

Y

Δ

Y

e

+

Y

Δ

Y

μ

+

Y

Δ

Y

τ

)

, measures the eﬃ-

c

iency in converting the lepton number asymmetries into the baryon number

R

e

f

erences 41

7

a

s

y

mmetr

y

.

S

inc

e

ε

1

α

and ˜

m

1

α

a

r

ese

n

s

i

t

i

ve to t

h

eﬂavo

r

st

r

uctu

r

eof

Y

ν

YY

,

t

h

e

p

rediction for the ﬁnal value of

Y

B

Y

i

sstron

g

ly model-dependent. This actually

s

igniﬁes the importance of ﬂavor eﬀects in a speciﬁc leptogenesis scenario.

I

t is wort

h

mentionin

g

t

h

at t

h

et

h

erma

l

corrections, spectator processes

a

nd quantum eﬀects in leptogenesis have also been considered

(

Buchm¨ulle

r

a

nd Fredenhagen, 2000; Buchm¨uller and Pl¨umacher, 2001; Giudic

e

et al

.

,

2

004

)

. In addition, CP violation in the decays of heavy Majorana neutrino

s

h

as recentl

y

been calculated in the non-equilibrium quantum ﬁeld theorie

s

(

Garn

y

et al.

, 2009, 2010a, 2010

b

;Bene

k

e

et al.

, 2010; Kießi

g

et al.

, 2010

)

.A

f

ull quantum-mechanical calculation o

f

the lepton number as

y

mmetr

y

based

on the Kadanoﬀ-Baym equations has also been done

(

Anisimo

v

e

tal

.

,

2010

).

It has been

f

ound that these improvements are likely to modi

f

y the previous

results by one order of magnitude in some cases

(

Anisimov

et al.

,

2010;

G

arn

y

et al.

,

2010a

).

R

e

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erence

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B

6

53, 278.

I

nde

x

A

a

b

so

l

ute

l

uminosit

y

,21

4

absolute magnitude, 214

apparent luminosity, 21

4

apparent ma

g

nitu

d

e, 214

A

skar

y

an eﬀect, 30

3

astronomical unit (AU), 21

3

atom

i

cmassun

i

t

,

22

0

B

baryon asymmetry of the Universe, 375

C

MB and BBN observations, 378

di

ﬀ

use

g

amma rays, 378

matter-antimatter annihilation

,

377

searches for antimatter, 37

6

b

eta

d

eca

y

,

2

bigbangnucleosynthesis

(

BBN

)

,

335

–

3

4

2

b

ar

y

on

d

ensit

y

,34

0

deuterium

,

337

deuterium abundance, 339

h

e

l

ium

,

337

helium mass

f

raction

,

338

lithium and beryllium, 337

l

it

h

ium

p

ro

bl

em, 340

neutrino s

p

ecies, 34

1

neutron-to-proton ratio, 33

6

big-bang model o

f

cosmology, 32

3

a

g

eo

f

the Universe, 327

critical energy density, 32

6

energy

d

ensities, 32

5

Frie

d

mann e

q

uations, 324

Hubble’s law, 32

4

c

osmological constant, 324

m

atter-

d

ominate

d

Universe

,

32

6

r

adiation-dominated Universe

,

325

r

adius of the Universe, 328

r

edshi

f

t

,

32

4

r

elativistic de

g

rees o

ff

reedom, 33

1

s

cale parameter, 32

4

th

eear

ly

Universe, 32

9

v

acuum-

d

ominate

d

Universe

,

326

B

orexino experiment, 67, 240

C

c

entimeter-gram-second

(

cgs

)

unit, 21

5

C

handrasekhar mass limit

,

252

C

herenkov radiation, 23

7

C

hern-

S

imons number

,

38

3

C

HOOZ ex

p

eriment, 68

C

OBE satellite, 34

9

c

oherent

f

orward scatterin

g

,4

3

c

ollective neutrino oscillations

,

272–28

4

b

ipolar oscillations, 272, 277–28

0

c

ritica

l

ener

g

y, 28

3

eq

uations o

f

motion, 27

3

ﬂ

avor pendulum, 27

7

g

eometrical

f

actor, 27

3

m

u

l

ti-an

gl

eca

l

cu

l

ation, 27

3

n

eutrino bulb model, 27

3

s

ing

l

e-ang

l

e approximation, 273

sp

ectra

l

s

pl

its, 280–283

s

ynchronized oscillations, 272

,

2

75

–2

77

t

hree-

ﬂ

avor e

ﬀ

ects

,

284

c

olor magnitude, 215

422 In

dex

co

l

or-ma

g

nitu

d

e

d

ia

g

ram, 215

constant neutr

i

no m

i

x

i

n

g

patterns, 10

0

d

emocratic mixin

g

matrix, 10

1

tetra-maxima

l

mixin

g

matrix, 102

tri-

b

imaxima

l

mixing matrix, 101

core-collapse supernovae, 252

delayed-shock explosion, 254

gravitational collapse, 25

3

photodissociation of heavy nuclei,

253

prompt-s

h

oc

k

exp

l

osion, 25

3

s

h

oc

k

wave, 25

3

son

i

cpo

i

nt, 253

cosmic microwave background

(

CMB

)

r

a

d

iation

,

290

,

349–35

9

acoustic

p

ea

k

s, 356

an

g

u

l

ar power spectrum, 35

4

an

i

sotropy, 353

b

aryon-p

h

oton equa

l

ity, 350

bound on neutrino masses, 359

decoupling time, 35

3

dipole, 354

Doppler shift, 355

integrated Sachs-Wolfe (ISW) eﬀect

,

356

last scattering surface, 35

3

matter-photon equality, 35

0

matter-radiation equality, 349

monopole, 354

multipoles, 355

number of neutrino species, 35

7

Planck s

p

acecraft, 35

9

recombination

,

35

1

WM

A

P satellite

,

353

cosmic neutrino background

(C

ν

B

)

,11

,

3

13, 342–34

7

capture on radioactive nuclei, 34

3

capture rate, 34

4

Cavendish-type torsion balance, 34

5

ex

p

erimenta

ld

etection, 34

3

steri

l

eneutrinos

,

345

S

todolsk

y

e

ﬀ

ect, 34

6

temperature an

d

num

b

er

d

ensit

y

,34

2

U

HE neutrinos an

d

Z

-b

ursts

,

346

cosm

i

cra

y

s, 290

a

ll

-

p

artic

l

es

p

ectrum, 29

0

D

dark matter (DM), 363–37

2

a

xions

,

36

4

c

old dark matter

(

CDM

)

, 364

g

ravitationa

ll

ensin

g

,36

3

h

ot DM

,

365

l

oca

ld

ensity, 36

4

n

on-baryonic dark matter, 36

3

p

rimordial black holes, 36

4

r

otation curves of galaxies, 363

s

terile neutrinos, 369

w

arm DM, 365

W

IMPs, 365

D

a

y

aBa

y

experiment, 20

7

d

egeneracy pressure of electrons, 250

d

ensit

y

matrix, 187–200

b

i

p

olar

ﬂ

avor conversions, 199

ﬂ

avor

p

olarization vector, 18

9

g

eometrica

ld

escription, 192

n

on-linear e

ﬀ

ects

,

19

5

t

hree-

ﬂ

avor oscillations

,

193

t

wo-

ﬂ

avor oscillations

,

18

8

d

i

ﬀ

use supernova neutrino backgroun

d

(

DSNB

)

, 260–26

1

c

onstraint

f

rom

S

Kex

p

eriment, 26

1

d

i

ﬀ

erential neutrino

ﬂ

ux

,

261

n

eutrino num

b

er

d

ensit

y

, 260

s

u

p

ernova rate,

261

d

iscrete spacetime s

y

mmetries, 79–86

C

, P and T trans

f

ormations, 7

9

c

onditions

f

or

C

P invariance, 85

C

P violation, 81

C

PT invariance, 81

E

e

l

ectric an

d

ma

g

netic

d

ipo

l

emoments,

89–9

2

m

assive Dirac neutrinos, 8

9

m

assive Majorana neutrinos, 9

1

electromagnetic

(

EM

)

form factors,

86

–

89

a

napole moment, 88

e

lectric dipole moment, 8

8

m

agnetic dipole moment, 8

8

m

assive Dirac neutrinos

,

8

m

assive Ma

j

orana neutrinos, 8

9

t

ransition

d

i

p

o

l

emoments,8

9

e

l

ectroma

g

netic neutrino-e

l

ectro

n

scattering, 94

c

ross section, 95

e

ﬀects of neutrino oscillations, 97

I

n

d

ex 42

3

ex

p

erimenta

l

constraints, 9

6

F

Fermi energy, 25

0

F

ermi momentum, 25

0

Fermi theor

y

,

3

Fierz trans

f

ormations

,

35

ﬁnite-temperature ﬁeld theor

y

,5

1

f

ermionic propa

g

ator, 55

scalar propagator, 54

two-

p

oint

G

reen

f

unctions, 52

ﬂavor distribution of UHE neutrinos

,

305

CPT violation

,

310

ﬂ

avor democracy, 308

general parametrization, 306

G

lashow resonance

,

30

8

muon-tau symmetry breakin

g

, 308

neutrino

d

eca

y

s, 311

quantum decoherence, 309

steri

l

eneutrinos

,

312

UHE neutrino oscillations, 30

5

unitarit

y

vio

l

ation, 31

0

working observables, 30

7

ﬂ

avor

p

uzzles, 10

5

Koide relation, 107

mass

h

ierarc

h

ies

,

106

quark-lepton complementarity, 10

8

ri

gh

tan

gl

es, 10

8

G

GALLEX

/

GNO experiment, 65, 23

7

G

amow

p

eak, 22

5

gauge invariance, 21–2

3

G

oldstone bosons

,

2

5

Greisen-Zatsepin-Kuzmin (GZK

)

c

uto

ﬀ

, 9, 290–29

2

Δ

r

esonance

,

29

0

energy t

h

res

h

o

ld

,29

1

GZK neutrinos

,

9

,

29

2

H

Higgs mechanism, 25

Hi

pp

arcos sate

ll

ite, 214

Homestake experiment, 65, 23

3

I

in

ﬂ

ation

,

360–36

3

density ﬂuctuations, 362

ﬂ

atness

p

roblem, 36

0

H

arrison-Ze

ld

ovic

h

s

p

ectrum, 36

2

h

orizon pro

bl

em, 361

m

agnetic monopole, 36

1

m

atter power spectrum, 36

2

sp

ectral index, 36

2

I

nternational System of units

(

SI

)

, 215

K

2K experiment, 63

K

amiokande experiment, 238

K

amLAND ex

p

eriment, 6

7

K

ubo-Martin-

S

chwin

g

er relation, 5

3

L

ane-Emden equation, 251

l

arge-scale structure (LSS), 363–36

9

c

onstraints on neutrino masses

,

369

d

ensit

yﬂ

uctuations o

fC

DM, 366

f

ree streamin

g

, 366

m

atter

p

ower s

p

ectrum, 36

7

n

eutrino fraction, 36

6

l

eptogenesis, 390–41

7

b

aryon number asymmetry, 40

7

B

oltzmann e

q

uations, 39

8

ch

emica

l

e

q

ui

l

i

b

rium, 406

c

onsistent su

b

traction

,

404

C

Pas

y

mmetries, 39

2

d

ecays an

d

inverse

d

ecays, 40

1

e

ﬀective neutrino masses, 407

e

ﬃciency factor, 40

8

ﬂ

avor eﬀects

,

415

i

nteraction rate

d

ensit

y

, 400

l

epton-num

b

er-vio

l

atin

g

scatterin

g,

404

n

on-t

h

erma

ll

epto

g

enesis, 392

s

el

f

-ener

g

y corrections, 39

3

th

erma

ll

epto

g

enesis, 391

v

ertex correct

i

ons, 395

l

epton number conservation, 7

1

l

epton number violation, 73, 38

2

l

eptonic unitarity violation, 150–155

J

ar

l

s

k

o

g

invariants, 15

1

n

on-unitar

yC

P violation, 15

2

l

ight year

(

ly

)

, 214

l

on

g

-

b

ase

l

ine neutrino experiments, 20

1

b

eta-beam facilities, 203

n

eutrino factories, 20

4

s

uper-beam facilities, 20

2

424 In

dex

M

Maki-Nakagawa-Sakata

(

MNS

)

mixing

m

atrix

,

9

8

classiﬁcation of

p

arametrizations, 98

Fritzsch-Xing

(

FX

)

parametrization,

1

00

standard parametrization, 99

mass-luminosity relation, 226

mean molecular weight, 22

0

mechanisms of baryogenesis, 379–39

0

Aﬄeck-Dine mechanism, 38

7

axial anomal

y

, 382

bar

y

on number violation, 38

2

electroweak baryogenesis, 38

0

e

l

ectrowea

kph

ase transition, 38

5

G

UT baryo

g

enesis, 386

l

epto

g

enesis, 38

9

l

e

p

ton num

b

er vio

l

ation, 38

2

S

akharov conditions

,

37

9

s

ph

a

l

eron, 384

MIN

OS

ex

p

eriment, 63

muon neutr

i

no

,6

N

natura

l

units

,

22

4

neutr

i

no

,

2

d

is

p

ersion re

l

ation, 5

1

e

ﬀ

ective potential, 47, 57

e

l

ectric c

h

arge, 12

h

e

l

icity, 4, 12

m

i

x

i

ng parameters, 69

refractive index, 46

self-energy in media, 5

6

species, 12

neutrino decoupling, 332–335

eﬀective number of neutrinos, 334

entropy conservation, 33

3

freeze-out temperature, 332

number density of relic neutrinos

,

334

neutrino hypothesis, 2

neutrino interactions, 3

4

–

43

neutrino-electron scattering, 3

5

neutrino-neutrino scattering, 39, 19

5

neutrino-nucleon interactions, 41

neutrino mass terms, 69–78

Dirac masses, 7

1

hybrid mass terms, 75

Majorana masses, 73

n

eutrino osci

ll

ation ex

p

eriments, 62–68

,

201–20

9

a

ccelerator neutrinos, 6

3

a

tmos

ph

eric neutrinos, 6

3

r

eactor neutrinos, 67, 206

s

o

l

ar neutrinos, 64

n

eutrino osci

ll

ations

,

160

a

diabatic condition, 16

7

ad

ia

b

atic osci

ll

ations, 164

ad

ia

b

aticit

y

parameter, 16

8

C

P and T violation, 163

L

andau-Zener

f

ormula, 171, 26

6

l

eve

l

-crossin

g

transition, 16

9

n

eutrino-antineutrino oscillations,

1

64

n

on-a

d

ia

b

atic osci

ll

ations

,

16

8

o

scillation lengths, 161

p

ara

d

oxes, 17

8

q

uantum co

h

erence, 177, 184

s

um rules, 173

t

hree-

ﬂ

avor oscillations

,

171

t

ransition

p

ro

b

a

b

i

l

ities, 161, 16

2

w

ave-packet approach, 182

W

ol

f

enstein-Mikhe

y

ev-

S

mirno

v

(

MSW

)

eﬀects, 16

6

n

eutrino telescopes, 299

I

ce

C

ube

,

30

0

K

M3NeT

,

30

0

n

eutrinoless double-beta decay

(0

ν

2

β

)

,

75

O

PER

A

ex

p

eriment, 64

P

alo Verde ex

p

eriment, 6

8

p

arallax second

(

parsec or pc

)

, 214

p

arit

y

vio

l

ation, 4

p

olytropic process, 25

1

Q

q

uantum chromodynamics (QCD), 2

3

q

uantum electrodynamics

(

QED

)

,21

R

r

a

d

iative neutrino

d

eca

y

s, 92–9

4

d

ecay rates, 92

e

xperimenta

lb

oun

d

s, 9

4

r

a

d

ius mo

d

u

l

us

,

21

4

r

enormalizability, 25–28

I

n

d

ex 42

5

renorma

l

ization

g

roup equations

(

RGEs

)

, 109–119

Dirac neutrino mass

p

arameters, 116

Ma

j

orana neutrino mass parameters,

11

1

one-loop RGEs, 109

rephasing invariants, 10

3

Jarlskog invariant, 10

3

oﬀ-diagonal asymmetries, 10

5

S

A

GE ex

p

eriment, 65, 23

7

seesaw mec

h

anisms, 75, 125–155

’

tHoo

f

t’s naturalness criterion, 134

collider signals, 137, 13

9

inverse seesaw, 14

1

multiple seesaw, 142

seesaw hierarchy problem, 13

3

seesaw naturalness problem, 13

4

type-

(

I+II

)

seesaw, 138

t

y

pe-I seesaw, 135

t

y

pe-II seesaw, 13

7

t

y

pe-III seesaw, 140

solar neutrino unit

(

SNU

)

,23

6

so

l

ar neutrinos

,

7

,

230–24

5

bound on neutrino li

f

etimes

,

24

5

b

oun

d

on neutrino ma

g

netic

m

oments

,

24

5

f

uture ex

p

eriments, 24

0

matter e

ﬀ

ects

,

24

2

so

l

ar neutrino osci

ll

ations

,

242

so

l

ar neutrino

p

ro

bl

em, 241

s

p

in-

ﬂ

avor oscillation, 24

4

sources o

f

UHE neutrinos

,

292

active galactic nuclei

(

AGN

)

, 292–29

4

gamma ray bursts

(

GRBs

)

, 294–29

5

optica

ll

yt

h

in sources, 29

5

superheavy dark matter, 298

top-down models, 29

7

topological defects, 298

weakly-interacting massive particle

s

(

WIMPs

)

,29

8

spontaneous symmetry

b

rea

k

ing, 23–25

standard electroweak model, 28

charged-current interactions, 3

3

neutral-current interactions, 3

3

fermion masses, 32

gauge boson masses, 31

Higgs boson, 31

H

i

gg

s

b

oson mass, 3

1

w

ea

k

mixin

g

an

gl

e, 31

Y

u

k

awa interactions

,

31

s

tandard solar model

(

SSM

)

,22

8

c

arbon-nitrogen-oxygen

(

CNO

)

cycle

,

23

1

p

rimordial chemical abundances, 229

p

roton-proton

(

pp

)

chain, 230

s

olar neutrino ﬂuxes

,

232

s

olar neutrino s

p

ectra, 233

s

tellar evolution

,

213–22

7

c

hemical com

p

osition, 221

dy

namical timescale, 218

e

ner

g

y conservation, 221

e

ner

g

y sources, 22

3

e

ner

g

y trans

f

er, 221

eq

uation o

f

state, 21

9

e

vo

l

ution e

q

uations, 22

3

hyd

rostatic equi

l

i

b

rium, 21

9

K

e

l

vin-He

l

m

h

o

l

tz timesca

l

e

,

21

8

n

uc

l

ear timesca

l

e

,

218

r

a

d

iative opacit

y

, 222

s

te

ll

ar

p

ara

ll

ax, 214

s

teri

l

eneutrinos

,

369–37

2

e

x

p

erimenta

ld

etection, 37

2

p

ro

d

uction, 369

r

a

d

iative

d

eca

y

, 371

w

arm

d

ar

k

matter

,

37

1

X

-ra

y

o

b

servations, 37

2

S

udbury Neutrino Observatory

(

SNO

)

experiment, 65, 23

9

S

uper-Kamiokande (SK) experiment

,

62

,

65

,

239

S

upernova 1987A

(

SN 1987A

)

,25

6

B

a

k

san experiment, 25

8

b

ound on neutrino lifetimes, 259

b

oun

d

on neutrino magneti

c

moments

, 260

b

oun

d

on neutrino masses

,

259

e

ner

g

y

l

oss ar

g

ument, 26

0

I

rvine-Michigan-Brookhaven

(

IMB

)

detector, 257

K

amiokande-II detector, 257

M

ont Blanc experiment, 259

s

upernova neutrinos, 8, 254–25

6

a

verage neutrino energy, 256

b

eta equilibrium, 254

d

eleptonization neutrino burst, 25

5

Xing Zh., Zhou Sh. Neutrinos in Particle Physics, Astronomy and Cosmology

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