Majoron Dark Matter and Constraints on the Majoron-Neutrino Coupling - - PowerPoint PPT Presentation

▶
majoron dark matter and constraints on the majoron
SMART_READER_LITE
LIVE PREVIEW

Majoron Dark Matter and Constraints on the Majoron-Neutrino Coupling - - PowerPoint PPT Presentation

Jan 29, 2024 44 likes •164 views

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 TIII / Singlet Majoron Model Physics Motivation What it is the origin of

slide-1
SLIDE 1

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

slide-2
SLIDE 2

Singlet Majoron Model

TIII / Physics

Motivation

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

The Majoron Model Chikashige, Mohapatra, and Peccei D. 1981

Majoron: Goldstone boson from spontaneous breaking of global U(1)B−L Small left-handed neutrino masses via Seesaw mechanism Majoron mass → dark matter? Constraints for mJ = 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 mJ = 0?

Brune and P¨

  • as. 2018. eprint: 1808.08158

Tim Brune, December 2018 1/10

slide-3
SLIDE 3

Singlet Majoron Model

TIII / Physics

Symmetry Breaking

Add three right-handed neutrinos NR and a singlet complex scalar σ , L(σ) = −2, to SM: L = −¯ LyNRH − 1 2 ¯ Nc

RλNRσ + h.c.

SSB at Seesaw-scale f: σ = 1 √ 2 (f + σ0 + iJ) L ⊃ −¯ LyNRH − 1 2 √ 2 ¯ Nc

RλNR f

  • mass term: MR= λf

√ 2

− i 2 √ 2 ¯ Nc

RλNR J

  • interaction

+h.c. SSB at electroweak scale v L ⊃ − ¯ νLyNRv

  • mass term: mD= yv

√ 2

− 1 2 √ 2 ¯ Nc

RλNRf

  • mass term: MR= λf

√ 2

− i 2 √ 2 ¯ Nc

RλNRJ

  • interaction

+h.c.

  • Pilaftsis. 1994

Tim Brune, December 2018 2/10

slide-4
SLIDE 4

Singlet Majoron Model

TIII / Physics

Seesaw Mechanism

Majorana mass MR = λf √ 2 , Dirac mass mD = yv √ 2 Neutrino masses in the Seesaw limit MR ≫ mD mheavy ≈ MR mlight ≈ − mDmT

D

MR ≪ MR Couplings of the Majoron to light neutrinos Llight

J

=

3

  • i

gii ¯ νiγ5νiJ

  • Minkowski. 1977

Tim Brune, December 2018 3/10

slide-5
SLIDE 5

Dark Matter

TIII / Physics

Majoron Dark Matter via Freeze-In

Explicit U(1)B−L breaking term → m2

J = λhv2

LH = λhσ2H†H + h.c. ⊃

  • SSB

− 1 2 m2

JJ2

  • 1 + h

v

  • Majoron relic density

ΩJh2 ≈ 2 1.09 × 1027 gs

∗

  • gρ

∗

mJΓ(h → JJ) m2

h

. Majoron DM: mJ ≈ 2.8 MeV For f ≈ 109 GeV: τJ > τuniverse → stable Hall et al. 2010 Frigerio, Hambye, and Masso. 2011

Tim Brune, December 2018 4/10

slide-6
SLIDE 6

Constraints

TIII / Physics

Supernova Constraints

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

Deleptonization Constraints

Successful SN explosion requires YL = Ye + Yνe ≥ 0.375 νeνe,α → J lower YL, α = µ, τ

  • Bruenn. 1985

Constraints on g(mJ) Luminosity Constraints

Model predictions are compatible with neutrino signal from SN1987A Neutrinos carry away most of the binding energy EB ≈ 3 · 1053 erg s Majoron carries away binding energy via νν → J Agreement with signal: Majoron luminosity LJ < Ltot

ν

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

  • Baksan. 1987

Tim Brune, December 2018 5/10

slide-7
SLIDE 7

Constraints

TIII / Physics

Supernova Constraints

1 10 100 1000 1013 1011 109 107 105

mJ MeV

gΑΒ

gΑΑ Luminosity gee Deleptonization gΑe Luminosity gee Luminosity

  • ✠

DM α = µ, τ Brune and P¨

  • as. 2018, see also Heurtier and Zhang. 2017

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

Tim Brune, December 2018 6/10

slide-8
SLIDE 8

Constraints

TIII / Physics

0νββJ Constraints

ΓJ = GJ(Q, Z, mJ)|gee(mJ)|2|MJ|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: GJ(mJ) → 0 as mJ → Q

see also Blum, 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

mJ MeV

0.2 0.4 0.6 0.8 1.0

G mJ G 0

48Ca 136Xe 100Mo 150Nd

NEMO-3. 48Ca. 2016, EXO-200. 136Xe. 2014, NEMO-3. 100Mo. 2014, NEMO-3. 150Nd. 2016 Tim Brune, December 2018 7/10

slide-9
SLIDE 9

Constraints

TIII / Physics

0νββJ Constraints

0.2 0.5 1.0 2.0

mJ MeV

106 105 104 0.001 0.01 0.1

gee

48Ca 136Xe 100Mo 150Nd

  • ✒

DM Brune and P¨

  • as. 2018, see also Blum, 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

slide-10
SLIDE 10

Constraints

TIII / Physics

Combined Constraints

0.2 0.5 1.0 2.0 5.0

mJ MeV

1013 1010 107 104 0.1

gee

48Ca

gee Luminosity

  • ✒

DM Brune and P¨

  • as. 2018

Tim Brune, December 2018 9/10

slide-11
SLIDE 11

Conclusion

TIII / Physics

Conclusion and Outlook

The Majoron can explain the origin of neutrino masses on the basis of spontaneous symmetry breaking of a global U(1)B−L If massive, the Majoron is a dark matter candidate For mJ ≈ 0.1 MeV − 1 GeV, a large range of couplings is excluded from SN data Neutrinoless double beta decay excludes couplings gee ≥ 10−4 for mJ ≈ 1 MeV Properly include background in 0νββJ limits for mJ > 0 Future 0νββJ experiments and observations of SN can exclude larger regions

Tim Brune, December 2018 10/10