DBD Lecture VIII - physics.umass.edu · M.J. Ramsey-Musolf U Mass Amherst ... Dine, asymmetric DM,...

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Lecture VIII: Cosmic Frontier Connections

ACFI NLDBD School 10/31-11/3 2017!

M.J. Ramsey-Musolf U Mass Amherst

http://www.physics.umass.edu/acfi/

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Lecture VIII Goals

•  Provide some background on leptogenesis in the broader context of baryogenesis

•  Discuss some implications of 0νββ-decay searches for leptogenesis

•  Provide some background on cosmological probes of neutrino mass**

•  Invite questions !

** Disclaimer: not my primary area of expertise

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Lecture VIII Outline

I.  Origin of Matter: Leptogenesis

II.  Neutrino Mass from Cosmology

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I. Origin of Matter: Leptogenesis

Symmetries & Cosmic History

Standard Model Universe

EW Symmetry Breaking: Higgs

QCD: n+p! nuclei

QCD: q+g! n,p…

Astro: stars, galaxies,..

10-35 s

10-11 s 10-5 s

~ 1 m

380k yr




BSM Physics?

QCD: n+p! nuclei

QCD: q+g! n,p…


10-35 s

10-11 s 10-5 s

~ 1 m

380k yr

The Origin of Matter

Explaining the origin, identity, and relative fractions of the cosmic energy budget is one of the most compelling motivations for physics beyond the Standard Model

Cosmic Energy Budget

Dark Matter

Dark Energy

68 %

27 %

5 %

Baryons Baryons

Cosmic Baryon Asymmetry

Big Bang Nucleosynthesis:

Light element abundances depend on YB

Cosmic Microwave Bcknd:

Shape of anisotropies depends on YB

uILi = (Su)ij umass

Lj (49)

uIRi = (Tu)ij umass

Rj (50)

dILi = (Sd)ij dmass

Lj (51)

dIRi = (Td)ij dmass

Rj (52)

VCKM

= S†uSd (53)

V LCKM

= S†uSd (54)

(55)

V RCKM

= T †uTd (56)

V RCKM

= T †uTd (57)

H1�body

=GFp

2

⌘

2mN

~� · ~r ⇢(~r) (58)

⌘ / GF sin � sin ✓1

sin ✓2

sin ✓3

(59)

dA(199Hg) = S S

(60)

= 2.8⇥ 10�4 fm�2

(61)

S = �1.4⇥ 10�8 e� fm3

YB =nB

s= (8.59 ± 0.11)⇥ 10�11

5




QCD: n+p! nuclei

QCD: q+g! n,p…


10-35 s

10-11 s 10-5 s

~ 1 m

380k yr

How did we go from nothing to something ?

BSM Physics?

Ingredients for Baryogenesis

•  B violation (sphalerons)

•  C & CP violation

•  Out-of-equilibrium or CPT violation





Standard Model BSM

✔

✖

✖

✔

✔

✔





Standard Model BSM

✔

✖

✖

✔

✔

✔

Scenarios: leptogenesis, EW baryogenesis, Afflek-Dine, asymmetric DM, cold baryogenesis, post-sphaleron baryogenesis…




QCD: n+p! nuclei

QCD: q+g! n,p…


?

Baryogenesis: When? CPV? SUSY? Neutrinos?

10-35 s

10-11 s 10-5 s

~ 1 m

380k yr




QCD: n+p! nuclei

QCD: q+g! n,p…


?

Baryogenesis: When? CPV? SUSY? Neutrinos?

EW Baryogenesis: testable w/ EDMs + colliders

10-35 s

10-11 s 10-5 s

~ 1 m

380k yr

Leptogenesis: look for ingred’s w/ νs: DBD, ν osc

Baryogenesis Scenarios E

nerg

y S

cale

(GeV

)

1012

Affleck Dine 109

10 2 10-1

Standard thermal lepto

Electroweak, resonant lepto, WIMPY baryo, ARS lepto…

Post-sphaleron, cold…

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What Questions Does It Address ?

•  Is the neutrino its own antiparticle ?

•  Why is there more matter than antimatter ?

•  Why are neutrino masses so small?

New heavy neutrino-like particle = its own anti-particle

“See saw mechanism” “Leptogenesis”

Heavy neutrino decays in early universe generate baryon asym

ν = ν

Neutrinos and the Origin of Matter

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m2 ⇡MN (37)

�(N ! `H) 6= �(N ! ¯`H⇤) (38)

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•  Heavy neutrinos decay out of equilibrium in early universe

•  Majorana neutrinos can decay to particles and antiparticles

•  Rates can be slightly different (CP violation)

•  Resulting excess of leptons over anti-leptons partially converted into excess of quarks over anti-quarks by Standard Model sphalerons


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m2 ⇡MN (37)

�(N ! `H) 6= �(N ! ¯`H⇤) (38)

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20


✓MX

�M

◆>> 1 (79)

gX << 1 (80)

U↵N ⇠ mD

MN

(81)

U↵N ⇠r

vL

vR

� m⌫

MN

(82)

+⇣NR, NR

⌘(83)

�L =

✓�+

p2 �+

�0 ��+

p2

◆(84)

mL ⇠ ghL h�0

Li (85)

mN ⇠ ghR h�0

Ri (86)

�N ⌘ �(NR ! `H) + �(NR ! ¯H⇤) =|h|28⇡

MN (87)

�N(z) =K

1

(z)

K2

(z)�N (88)

H(T ) ⇠ 1.66 g⇤T 2

MP

(89)

�(`H ! NR)

MN

(90)

H(T )

MN

(91)

7

NR

H

l h

Hubble rate

✓MX

�M

◆>> 1 (79)

gX << 1 (80)

U↵N ⇠ mD

MN

(81)

U↵N ⇠r

vL

vR

� m⌫

MN

(82)

+⇣NR, NR

⌘(83)

�L =

✓�+

p2 �+

�0 ��+

p2

◆(84)

mL ⇠ ghL h�0

Li (85)

mN ⇠ ghR h�0

Ri (86)

�N ⌘ �(NR ! `H) + �(NR ! ¯H⇤) =|h|28⇡

MN (87)

�N(z) =K

1

(z)

K2

(z)�N (88)

H(T ) ⇠ 1.66 g⇤T 2

MP

(89)

�(`H ! NR)

MN

(90)

H(T )

MN

(91)

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+ NR

H*

l h

_


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Simple estimation

2 4 6 8 10

0.2

0.4

0.6

0.8

✓MX

�M

◆>> 1 (79)

gX << 1 (80)

U↵N ⇠ mD

MN

(81)

U↵N ⇠r

vL

vR

� m⌫

MN

(82)

+⇣NR, NR

⌘(83)

�L =

✓�+

p2 �+

�0 ��+

p2

◆(84)

mL ⇠ ghL h�0

Li (85)

mN ⇠ ghR h�0

Ri (86)

�N ⌘ �(NR ! `H) + �(NR ! ¯H⇤) =|h|28⇡

MN (87)

�N(z) =K

1

(z)

K2

(z)�N (88)

H(T ) ⇠ 1.66 g⇤T 2

MP

(89)

�(`H ! NR)

MN

(90)

H(T )

MN

(91)

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ΓN (z

) / Γ

N

z = MN / T

ΓN < H(T=MN )~


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Simple estimation

Lmass

=�

⌫L NCR

� ✓0 mD

mD MN

◆ ✓⌫L

NR

◆(37)

m1

⇡ m2

D

MN

(38)

m2

⇡ MN (39)

Lmass

=�

⌫L NCR

� ✓0 mD

mD MN

◆ ✓⌫L

NR

◆+ mL⌫C

L ⌫L (40)

Lmass

=�

⌫L NR NCS

�0

@0 mL

D 0mL

D 0 MRD

0 MRD µ

1

A

0

@⌫L

NR

NS

1

A (41)

m⌫ ⇠ mLD

�MR

D

��1

µ�MR

D

��1

mLD (42)

�(N ! `H) 6= �(N ! ¯H⇤) (43)

Lmass

= yLHNR + h.c. + MNNCR NR (44)

Lmass

=y

⇤LcHHT L + h.c. (45)

�(NR ! `H) 6= �(NR ! ¯H⇤) (46)

m⌫ =m2

D

MR

(47)

hp0| JEM

µ |pi = U(p0)

F

1

�µ +iF

2

2M�µ⌫q

⌫ +iF

3

2M�µ⌫�5

q⌫ +FA

M2

(q2�µ � 6qqµ)�5

�U(p) (48)

4

m⇤ = 8⇡ ⇤ (1.66g⇤)v2

MP

(92)

8

~ few x 10-3 eV

m⇤ = 8⇡ ⇤ (1.66g⇤)v2

MP

(92)

m1

⇡ m⇤ (93)

8

ΓN < H(T=MN )~


23


Washout processes

NR

H * H

l l _

ΔL = 2


24


Complete calculation: Boltzmann equations

di Bari ‘12

Non-Eq: T < mN

Eq: T > mN


25

m2 ⇡MN (37)

�(N ! `H) 6= �(N ! ¯`H⇤) (38)

4






26

m2 ⇡MN (37)

�(N ! `H) 6= �(N ! ¯`H⇤) (38)

4






27

CPV Asymmetry

Tree-level CPV One-loop “absoprtive part” X

Buchmuller, Peccei, Yanagida ‘05


28

CPV Asymmetry

Tree-level CPV One-loop “absoprtive part” X


CPV phases but not same as φPMNS


29

Putting pieces together: B-L asymmetry



30

m2 ⇡MN (37)

�(N ! `H) 6= �(N ! ¯`H⇤) (38)

4





Electroweak Sphalerons

31

Aλ

Sphaleron Configuration


32

Aλ

Sphaleron Configuration Δ (B+L) / NFAnomaly


33

Aλ

Sphaleron Configuration Δ (B+L) / NFAnomaly

EW sphalerons convert B-L asymmetry to YB

Davidson-Ibarra Bound

34

m⇤ = 8⇡ ⇤ (1.66g⇤)v2

MP

(92)

m1

⇡ m⇤ (93)

1

T1/2

= G0⌫(E,Z) |M0⌫ | |hm��i|2 (94)

Lfs

/ m�1/2

⌫ (95)

|✏1

| <⇠3

8⇡

MN1

m⌫3

hH0i2 (96)

8

MN1 > 109 GeV ~

Davidson, Ibarra ‘02

35

TeV Scale LNV ?

€

e−

€

e−

€

A Z,N( )

€

A Z − 2,N + 2( )

TeV LNV Mechanism

Dirac Majorana

O5 =

��H

⇤

�� H†H (25)

M⌃± �M⌃0 ⇠ ↵

4⇡MW (26)

L =

g

2

hij

⇥¯LCi"�LLj

⇤+ (L$ R) + h.c. (27)

��Qe

W

QeW

�� = 0.14

|hee|2(M�/1 TeV)

2 (28)

|Vud|2 + |Vus|2 = |Vud|21 +

|Vus|2|Vud|2

�(29)

Lmass = y ¯L ˜H⌫R + h.c. (30)

Lmass =

y

⇤

¯Lc˜H ˜HT L + h.c. (31)

3

O5 =

��H

⇤

�� H†H (25)

M⌃± �M⌃0 ⇠ ↵

4⇡MW (26)

L =

g

2

hij

⇥¯LCi"�LLj

⇤+ (L$ R) + h.c. (27)

��Qe

W

QeW

�� = 0.14

|hee|2(M�/1 TeV)

2 (28)

|Vud|2 + |Vus|2 = |Vud|21 +

|Vus|2|Vud|2

�(29)

Lmass = y ¯L ˜H⌫R + h.c. (30)

Lmass =

y

⇤

¯LcHHT L + h.c. (31)

�(⌫R ! `H) 6= �(⌫R ! ¯`H⇤) (32)

m⌫ =

m2D

MR

(33)

3

33

F

B B

O(1) for Λ ~ 1 TeV

Implications

TeV LNV & Leptogenesis E

nerg

y S

cale

(GeV

)

1012

10 3

10 2 10-1


Fast ΔL = 2 int: erase L

36

Deppisch et al ‘14, ‘15

TeV LNV & Leptogenesis E

nerg

y S

cale

(GeV

)

1012

10 3

10 2 10-1


Electroweak, resonant lepto, WIMPY baryo, ARS lepto…

Post-sphaleron, cold…

Baryogenesis alternatives 37

Fast ΔL = 2 int: erase L Deppisch et al ‘14, ‘15

38

Low Scale “ARS” Leptogenesis

Akhmedov, Rubakov, Smirmov ‘98

1.  3 Singlet RH neutrinos: NA , NB , NC

2.  LTOT = LSM + LA + LB + LC

3.  Nk oscillations + CPV ! LA = 0, LA = 0, LA = 0 but LTOT =0

4.  Yukawa interactions: Lk , H + lk in equilibrium above TEW for k=A,B but not for k=C

5.  Lepton number for lA,B converted to nB by EW sphalerons

6.  Conditions 4 ! MNk can be ~ O( GeV )

/ / /

39

Low Scale “ARS” Leptogenesis

M. Drewes

40

II. Neutrino Mass from Cosmology

41

ACFI Workshop

December 2015

42

0νββ-Decay: Standard MechanismThree active light neutrinos

Effe

ctiv

e D

BD

neu

trino

mas

s (e

V)

Inverted Normal

Lightest neutrino mass (eV) !

43

0νββ-Decay: Standard Mechanism Three active light neutrinos

Effe

ctiv

e D

BD

neu

trino

mas

s (e

V)

Inverted Normal

Current generation Current generation

Ton Scale


44

0νββ-Decay: Standard Mechanism Three active light neutrinos

Effe

ctiv

e D

BD

neu

trino

mas

s (e

V)

Inverted Normal

Ton Scale

Full implications require information on lightest mass & hierarchy



45

Interpreting a Positive Result Three active light neutrinos

Effe

ctiv

e D

BD

neu

trino

mas

s (e

V)

Inverted Normal

Ton Scale

Positive result would be consistent with 3 light active ν’s & IH or quasi-deg regime, but not definitive as to mechanism



46

Interpreting a Null Result: St’d Mechanism Three active light neutrinos

Effe

ctiv

e D

BD

neu

trino

mas

s (e

V)

Inverted Normal

Ton Scale

Full implications require information on lightest mass & hierarchy



47

Kinematic Neutrino Mass Measurements

KATRIN 3H ! 3He e- ν _

48

St’d Mech: What Would a Null Result Imply ? Three active light neutrinos

Effe

ctiv

e D

BD

neu

trino

mas

s (e

V)

Inverted Normal

Ton Scale

3H decay cur gen

Null result in NLDBD & non-zero mν from 3H decay ! Neutrinos are (pseudo) Dirac



49



Effe

ctiv

e D

BD

neu

trino

mas

s (e

V)

Inverted

Ton Scale

3H decay cur gen

Normal

3H decay next gen



50



Effe

ctiv

e D

BD

neu

trino

mas

s (e

V)

Inverted

Ton Scale

Normal



3H decay cur gen

3H decay next gen

P. Vogel

51

Neutrino Mass & Cosmology

Matter Power Spectrum

Transition to non-rel ν matter

Massive neutrinos suppress power (relative to large scale power) at scales below free streaming scale K. Abazajian ACFI neutrino mass workshop

Σ mv < 0.12 eV

52



K. Abazajian ACFI neutrino mass workshop

J. Brau, U. Oregon

Later Earlier

53




Later Earlier

Neutrino Free Streaming

ΩM = Ων + ΩDM + ΩB δρν δρDM

Free Streaming Scale

m⇤ = 8⇡ ⇤ (1.66g⇤)v2

MP

(92)

m1

⇡ m⇤ (93)

1

T1/2

= G0⌫(E,Z) |M0⌫ | |hm��i|2 (94)

Lfs

/ m�1/2

⌫ (95)

8

54




Later Earlier




m⇤ = 8⇡ ⇤ (1.66g⇤)v2

MP

(92)

m1

⇡ m⇤ (93)

1

T1/2

= G0⌫(E,Z) |M0⌫ | |hm��i|2 (94)

Lfs

/ m�1/2

⌫ (95)

8

δρν (power) suppressed for L < Lfs

55




Later Earlier




m⇤ = 8⇡ ⇤ (1.66g⇤)v2

MP

(92)

m1

⇡ m⇤ (93)

1

T1/2

= G0⌫(E,Z) |M0⌫ | |hm��i|2 (94)

Lfs

/ m�1/2

⌫ (95)

8


Suppression moves to smaller scales ! Larger k

Increase mν

56







m⇤ = 8⇡ ⇤ (1.66g⇤)v2

MP

(92)

m1

⇡ m⇤ (93)

1

T1/2

= G0⌫(E,Z) |M0⌫ | |hm��i|2 (94)

Lfs

/ m�1/2

⌫ (95)

8


Suppression moves to smaller scales ! Larger k

Increase mν

Later Earlier

Increase mν

Σ mv < 0.12 eV Palanque-Dalabrouille ‘15

57



Effe

ctiv

e D

BD

neu

trino

mas

s (e

V)

Inverted

Ton Scale

3H decay cur gen

Null result in NLDBD & non-zero mν from cosmology ! Conclusion depends on mlightest & hierarchy

Normal

3H decay next gen

Cosmo current


58



Effe

ctiv

e D

BD

neu

trino

mas

s (e

V)

Inverted

Ton Scale

3H decay cur gen

Null result in NLDBD & non-zero mν from cosmology ! Conclusion depends on mlightest & hierarchy

Normal


Cosmo current

3H decay next gen

P. Vogel

59

Lecture VIII Summary •  Simplest type I see-saw mechanism with Majorana 3 NR + CPV

provides ingredients for baryogenesis via thermal leptogenesis

•  “Standard leptogenesis” ! MN1 > 109 GeV

•  Observation of 0νββ-decay consistent with “standard mechanism” would demonstrate existence of one key ingredient for thermal leptogenesis

•  Discovery of TeV scale (and below) LNV (0νββ-decay + LHC…) would preclude high scale leptogenesis & point to alternate, low-scale scenarios (ARS lepto, EW baryo…)

•  Precision cosmology (large scale structure, CMB) places tight constraints on Σmν for the three light active neutrinos, squeezing the viability of the IH region for mββ

•  Challenge for theory: are there any well-motivated loopholes to cosmological constraints ?

DBD Lecture VIII - physics.umass.edu · M.J. Ramsey-Musolf U Mass Amherst ... Dine, asymmetric DM,...

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Transcript of DBD Lecture VIII - physics.umass.edu · M.J. Ramsey-Musolf U Mass Amherst ... Dine, asymmetric DM,...