Majoron Dark Matter and Constraints on the Majoron-Neutrino Coupling

TIII / Physics

Majoron Dark Matter and Constraints on the Majoron-Neutrino Coupling

Tim Brune The quest for new physics

December 2018

Tim Brune, December 2018

Singlet Majoron Model

Motivation

What it is the origin of (small) neutrino masses?

What is dark matter?

The Majoron Model

Majoron: Goldstone boson from spontaneous breaking of globalU(1)B−L

Small left-handed neutrino masses via Seesaw mechanism Majoron mass→ dark matter?

Constraints form_J =0:Kachelriess, Tomas, and Valle.2000,Tomas, P ¨as, and Valle.2001 Constraints on non-standard Majoron models:Cepedello et al.2018

Constraints on Majoron-Neutrino couplings from SN data and 0νββJ for m

6= 0?

Brune and P ¨as.2018. eprint:1808.08158

Singlet Majoron Model

Symmetry Breaking

Add three right-handed neutrinosNRand a singlet complex scalarσ ,L(σ) =−2, to SM:

L=−LyN¯ _RH−1 2

N¯_R^cλN_Rσ+h.c.

SSB at Seesaw-scalef:σ= 1

√

2(f+σ⁰+iJ) L ⊃ −LyN¯ RH− 1

2√ 2

N¯_R^cλNR f

| {z }

mass term:M_R=√^λf 2

− i 2√

2

N¯_R^cλNR J

| {z }

interaction

+h.c.

SSB at electroweak scalev L ⊃ − ν¯LyNRv

| {z }

mass term:m_D=√^yv 2

− 1 2√ 2

N¯_R^cλNRf

| {z }

mass term:M_R=√^λf 2

− i 2√

2 N¯_R^cλNRJ

| {z }

interaction

+h.c.

Pilaftsis.1994

Tim Brune, December 2018 2/10

Singlet Majoron Model

Seesaw Mechanism

Majorana massM_R= λf

√

2, Dirac massm_D= yv

√ 2 Neutrino masses in the Seesaw limitMRmD

m_heavy≈M_R m_light≈ −m_Dm_D^T M_R M_R Couplings of the Majoron to light neutrinos

L^light_J =

3

X

i

giiν¯iγ5νiJ

Minkowski.1977

Dark Matter

Majoron Dark Matter via Freeze-In

ExplicitU(1)_B−Lbreaking term→m²_J=λhv²

L_H =λ_hσ²H^†H+h.c. ⊃

|{z}

SSB

−1 2m²_JJ²

1+h

v

Majoron relic density

ΩJh²≈21.09×10²⁷ g^s∗

pg^ρ∗

m_JΓ(h→JJ) m²_h . Majoron DM:m_J≈2.8 MeV

Forf ≈10⁹GeV:τ_J > τ_universe→stable

Hall et al.2010

Frigerio, Hambye, and Masso.2011

Tim Brune, December 2018 4/10

Constraints

Supernova Constraints

In the SN core: neutrinos acquire effective masses due to interactions with the background medium⇒νν→Jis allowed

Deleptonization Constraints

Successful SN explosion requires YL=Ye+Yν_e ≥0.375

νeνe,α→JlowerYL,α=µ, τ Bruenn.1985

Constraints on g(m

)

Luminosity Constraints

Model predictions are compatible with neutrino signal from SN1987A Neutrinos carry away most of the binding energyE_B≈3·10⁵³erg s Majoron carries away binding energy via νν→J

Agreement with signal: Majoron luminosityL_J <L^tot_ν

Similar aprroach:Heurtier and Zhang.2017 Data:Kamiokande-II.1987,IMB.1987, Baksan.1987

Constraints

Supernova Constraints

1 10 100 1000

10^-13 10^-11 10^-9 10^-7 10^-5

mJ

MeV

È g

È

ÈgeeÈDeleptonization ÈgΑeÈLuminosity ÈgeeÈLuminosity DM

α=µ, τ

Brune and P ¨as.2018, see alsoHeurtier and Zhang.2017

Data:Kamiokande-II.1987,IMB.1987,Baksan.1987,Bruenn.1985

Tim Brune, December 2018 6/10

Constraints

0νββJ Constraints

Γ^J=G^J(Q,Z,m_J)|gee(m_J)|²|M^J|²

dL uL

e⁻ J e⁻

dL uL

W

ν

W

dL uL

e⁻ J e⁻

dL uL

W

ν

W

Georgi, Glashow, and Nussinov.1981 Constraints:

Reduced signal-to-background ratio Decreasing phase space:

G^J(m_J)→0 asm_J→Q see alsoBlum, Nir, and Shavit.2018

0.0 0.5 1.0 1.5 2.0 2.5 3.0

T MeV

0.2 0.4 0.6 0.8 1.0 1.2

a.u.

0ΝΒΒJ, mJ=0 0ΝΒΒJ, mJ=me 0ΝΒΒJ, mJ=2me 0ΝΒΒJ, mJ=3me 0ΝΒΒJ, mJ=4me 2ΝΒΒ

1 2 3 4

m_J MeV

0.2 0.4 0.6 0.8 1.0

GHmJL GH0L

48Ca 136Xe 100Mo 150Nd

NEMO-3.48Ca. 2016,EXO-200.136Xe. 2014,NEMO-3.100Mo. 2014, NEMO-3.150Nd. 2016

Constraints

0νββJ Constraints

0.2 0.5 1.0 2.0

m_J

10^-6 MeV

10^-5 10^-4 0.001 0.01 0.1

È g

È

48Ca

136Xe

100Mo

150Nd

DM

Brune and P ¨as.2018, see alsoBlum, Nir, and Shavit.2018

Data:NEMO-3.⁴⁸Ca. 2016,EXO-200.¹³⁶Xe. 2014,NEMO-3.¹⁰⁰Mo. 2014,NEMO-3.¹⁵⁰Nd. 2016

Tim Brune, December 2018 8/10

Constraints

Combined Constraints

0.2 0.5 1.0 2.0 5.0

mJ 10^-13 MeV

10^-10 10^-7 10^-4 0.1

È g

È

48Ca Èg_eeÈLuminosity DM

Brune and P ¨as.2018

Conclusion

Conclusion and Outlook

The Majoron can explain the origin of neutrino masses on the basis of spontaneous symmetry breaking of a global U(1)

If massive, the Majoron is a dark matter candidate

For m

≈ 0.1 MeV − 1 GeV, a large range of couplings is excluded from SN data

Neutrinoless double beta decay excludes couplings g

≥ 10

for m

≈ 1 MeV

Properly include background in 0νββJ limits for m

> 0

Future 0νββJ experiments and observations of SN can exclude larger regions

Tim Brune, December 2018 10/10