Manifestations of Low-Mass Dark Bosons Yevgeny Stadnik Humboldt - - PowerPoint PPT Presentation

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Manifestations of Low-Mass Dark Bosons Yevgeny Stadnik Humboldt - - PowerPoint PPT Presentation

Sep 25, 2022 227 likes •803 views

Manifestations of Low-Mass Dark Bosons Yevgeny Stadnik Humboldt Fellow Johannes Gutenberg University, Mainz, Germany Collaborators (Theory): Victor Flambaum (UNSW) Collaborators (Experiment): CASPEr collaboration at Mainz nEDM collaboration

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Yevgeny Stadnik

Humboldt Fellow

Beyond Standard Model: Where do we go from here?, Florence, September 2018

Manifestations of Low-Mass Dark Bosons

Collaborators (Theory): Victor Flambaum (UNSW) Collaborators (Experiment): CASPEr collaboration at Mainz nEDM collaboration at PSI and Sussex BASE collaboration at CERN and RIKEN

Johannes Gutenberg University, Mainz, Germany

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“Low-mass” (m << 100 GeV) dark bosons may explain several outstanding puzzles

Motivation for Low-Mass Dark Bosons

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Dark Matter

Overwhelming astrophysical evidence for existence

  • f dark matter (~5 times more dark matter than
  • rdinary matter).

ρDM ≈ 0.4 GeV/cm3 vDM ~ 300 km/s

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SLIDE 4

“Low-mass” (m << 100 GeV) dark bosons may explain several outstanding puzzles:

  • Dark matter and dark energy
  • Strong CP problem
  • Hierachy problem
  • ‘Hints’ of temporal and spatial variations of the

electromagnetic fine-structure constant α at z ~ 1

⋮

Motivation for Low-Mass Dark Bosons

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SLIDE 5

Manifestations of Dark Bosons

New forces Interconversion with

  • rdinary particles

Stellar emission Dark matter

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SLIDE 6

Manifestations of Dark Bosons

New forces Interconversion with

  • rdinary particles

Stellar emission Dark matter

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SLIDE 7

Manifestations of Dark Bosons

New forces Interconversion with

  • rdinary particles

Stellar emission Dark matter

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SLIDE 8

Electric Dipole Moment (EDM) = parity (P) and time-reversal- invariance (T) violating electric moment

Basics of Atomic EDMs

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Electric Dipole Moment (EDM) = parity (P) and time-reversal- invariance (T) violating electric moment

Basics of Atomic EDMs

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Electric Dipole Moment (EDM) = parity (P) and time-reversal- invariance (T) violating electric moment

Basics of Atomic EDMs

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|d Hg| limit ≈ 7*10-30 e cm

Sensitivity of EDM Experiments

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|d Hg| limit ≈ 7*10-30 e cm

Sensitivity of EDM Experiments

LHg ≈ 3*10-8 cm

+δQ

  • δQ

(dHg)classical = δQ·LHg

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SLIDE 13

|d Hg| limit ≈ 7*10-30 e cm

Sensitivity of EDM Experiments

LHg ≈ 3*10-8 cm

+δQ

  • δQ

δQ sensitivity ~ 10-22 e (!)

(dHg)classical = δQ·LHg

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SLIDE 14

[Stadnik, Dzuba, Flambaum, PRL 120, 013202 (2018)], [Dzuba, Flambaum, Samsonov, Stadnik, PRD 98, 035048 (2018)]

Non-Cosmological Sources of Dark Bosons

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SLIDE 15

P,T-violating forces => Atomic and Molecular EDMs

Non-Cosmological Sources of Dark Bosons

[Stadnik, Dzuba, Flambaum, PRL 120, 013202 (2018)], [Dzuba, Flambaum, Samsonov, Stadnik, PRD 98, 035048 (2018)]

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Atomic EDM experiments: Cs, Tl, Xe, Hg, Ra Molecular EDM experiments: YbF, HfF+, ThO

P,T-violating forces => Atomic and Molecular EDMs

Non-Cosmological Sources of Dark Bosons

[Stadnik, Dzuba, Flambaum, PRL 120, 013202 (2018)], [Dzuba, Flambaum, Samsonov, Stadnik, PRD 98, 035048 (2018)]

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SLIDE 17

Constraints on Scalar-Pseudoscalar Electron-Electron Interaction

EDM constraints: [Stadnik, Dzuba, Flambaum, PRL 120, 013202 (2018)] Many orders of magnitude improvement!

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Manifestations of Dark Bosons

New forces Interconversion with

  • rdinary particles

Stellar emission Dark matter

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SLIDE 19

Motivation

Traditional “scattering-off-nuclei” searches for heavy

WIMP dark matter particles (mχ ~ GeV) have not yet produced a strong positive result.

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SLIDE 20

Motivation

Traditional “scattering-off-nuclei” searches for heavy

WIMP dark matter particles (mχ ~ GeV) have not yet produced a strong positive result.

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SLIDE 21

Motivation

Traditional “scattering-off-nuclei” searches for heavy

WIMP dark matter particles (mχ ~ GeV) have not yet produced a strong positive result.

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SLIDE 22

Motivation

Traditional “scattering-off-nuclei” searches for heavy

WIMP dark matter particles (mχ ~ GeV) have not yet produced a strong positive result.

Challenge: Observable is fourth power in a small

interaction constant (eי << 1)!

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SLIDE 23

Motivation

Traditional “scattering-off-nuclei” searches for heavy

WIMP dark matter particles (mχ ~ GeV) have not yet produced a strong positive result.

Question: Can we instead look for effects of dark matter

that are first power in the interaction constant?

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Low-mass Spin-0 Dark Matter

  • Low-mass spin-0 particles form a coherently oscillating

classical field φ(t) = φ0 cos(mφc2t/ℏ), with energy density <ρφ> ≈ mφ

2φ0 2/2 (ρDM,local ≈ 0.4 GeV/cm3)

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SLIDE 25

Low-mass Spin-0 Dark Matter

  • Low-mass spin-0 particles form a coherently oscillating

classical field φ(t) = φ0 cos(mφc2t/ℏ), with energy density <ρφ> ≈ mφ

2φ0 2/2 (ρDM,local ≈ 0.4 GeV/cm3)

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SLIDE 26

Low-mass Spin-0 Dark Matter

  • Low-mass spin-0 particles form a coherently oscillating

classical field φ(t) = φ0 cos(mφc2t/ℏ), with energy density <ρφ> ≈ mφ

2φ0 2/2 (ρDM,local ≈ 0.4 GeV/cm3)

H >> mφ: φ ≈ const. => ρ ≈ const. [Dark energy regime]

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SLIDE 27

Low-mass Spin-0 Dark Matter

  • Low-mass spin-0 particles form a coherently oscillating

classical field φ(t) = φ0 cos(mφc2t/ℏ), with energy density <ρφ> ≈ mφ

2φ0 2/2 (ρDM,local ≈ 0.4 GeV/cm3)

H >> mφ: φ ≈ const. => ρ ≈ const. [Dark energy regime] H << mφ: φ ∝ cos(mφt)/t 3/4 => ρ ∝ 1/V [Cold DM regime]

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Low-mass Spin-0 Dark Matter

  • Low-mass spin-0 particles form a coherently oscillating

classical field φ(t) = φ0 cos(mφc2t/ℏ), with energy density <ρφ> ≈ mφ

2φ0 2/2 (ρDM,local ≈ 0.4 GeV/cm3)

  • Coherently oscillating field, since cold (Eφ ≈ mφc2)
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SLIDE 29

Low-mass Spin-0 Dark Matter

  • Low-mass spin-0 particles form a coherently oscillating

classical field φ(t) = φ0 cos(mφc2t/ℏ), with energy density <ρφ> ≈ mφ

2φ0 2/2 (ρDM,local ≈ 0.4 GeV/cm3)

  • Coherently oscillating field, since cold (Eφ ≈ mφc2)
  • Classical field for mφ << 1 eV, since nφ(λdB,φ
/2π)3 >> 1
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SLIDE 30

Low-mass Spin-0 Dark Matter

  • Low-mass spin-0 particles form a coherently oscillating

classical field φ(t) = φ0 cos(mφc2t/ℏ), with energy density <ρφ> ≈ mφ

2φ0 2/2 (ρDM,local ≈ 0.4 GeV/cm3)

  • Coherently oscillating field, since cold (Eφ ≈ mφc2)
  • Classical field for mφ << 1 eV, since nφ(λdB,φ
/2π)3 >> 1
  • Coherent + classical DM field = “Cosmic laser field”
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SLIDE 31

Low-mass Spin-0 Dark Matter

  • Low-mass spin-0 particles form a coherently oscillating

classical field φ(t) = φ0 cos(mφc2t/ℏ), with energy density <ρφ> ≈ mφ

2φ0 2/2 (ρDM,local ≈ 0.4 GeV/cm3)

  • Coherently oscillating field, since cold (Eφ ≈ mφc2)
  • Classical field for mφ << 1 eV, since nφ(λdB,φ
/2π)3 >> 1
  • Coherent + classical DM field = “Cosmic laser field”
  • 10-22 eV ≲ mφ << 1 eV <=> 10-8 Hz ≲ f << 1014 Hz

λdB,φ ≤ L dwarf galaxy ~ 1 kpc Classical field

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SLIDE 32

Low-mass Spin-0 Dark Matter

  • Low-mass spin-0 particles form a coherently oscillating

classical field φ(t) = φ0 cos(mφc2t/ℏ), with energy density <ρφ> ≈ mφ

2φ0 2/2 (ρDM,local ≈ 0.4 GeV/cm3)

  • Coherently oscillating field, since cold (Eφ ≈ mφc2)
  • Classical field for mφ << 1 eV, since nφ(λdB,φ
/2π)3 >> 1
  • Coherent + classical DM field = “Cosmic laser field”
  • 10-22 eV ≲ mφ << 1 eV <=> 10-8 Hz ≲ f << 1014 Hz
  • mφ ~ 10-22 eV <=> T ~ 1 year

λdB,φ ≤ L dwarf galaxy ~ 1 kpc Classical field

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SLIDE 33

Low-mass Spin-0 Dark Matter

  • Low-mass spin-0 particles form a coherently oscillating

classical field φ(t) = φ0 cos(mφc2t/ℏ), with energy density <ρφ> ≈ mφ

2φ0 2/2 (ρDM,local ≈ 0.4 GeV/cm3)

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SLIDE 34

Low-mass Spin-0 Dark Matter

  • Low-mass spin-0 particles form a coherently oscillating

classical field φ(t) = φ0 cos(mφc2t/ℏ), with energy density <ρφ> ≈ mφ

2φ0 2/2 (ρDM,local ≈ 0.4 GeV/cm3)

  • 10-22 eV ≲ mφ << 1 eV inaccessible to traditional “scattering-
  • ff-nuclei” searches, since |pφ| ~ 10-3mφ is extremely small

=> recoil effects of individual particles suppressed

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SLIDE 35

Low-mass Spin-0 Dark Matter

  • Low-mass spin-0 particles form a coherently oscillating

classical field φ(t) = φ0 cos(mφc2t/ℏ), with energy density <ρφ> ≈ mφ

2φ0 2/2 (ρDM,local ≈ 0.4 GeV/cm3)

  • 10-22 eV ≲ mφ << 1 eV inaccessible to traditional “scattering-
  • ff-nuclei” searches, since |pφ| ~ 10-3mφ is extremely small

=> recoil effects of individual particles suppressed

  • BUT can look for coherent effects of a low-mass DM field in

low-energy atomic and astrophysical phenomena that are first power in the interaction constant κ :

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SLIDE 36

Low-mass Spin-0 Dark Matter

  • Low-mass spin-0 particles form a coherently oscillating

classical field φ(t) = φ0 cos(mφc2t/ℏ), with energy density <ρφ> ≈ mφ

2φ0 2/2 (ρDM,local ≈ 0.4 GeV/cm3)

  • 10-22 eV ≲ mφ << 1 eV inaccessible to traditional “scattering-
  • ff-nuclei” searches, since |pφ| ~ 10-3mφ is extremely small

=> recoil effects of individual particles suppressed

  • BUT can look for coherent effects of a low-mass DM field in

low-energy atomic and astrophysical phenomena that are first power in the interaction constant κ :

  • First-power effects => Improved sensitivity to certain DM

interactions by up to 15 orders of magnitude (!)

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SLIDE 37

Low-mass Spin-0 Dark Matter

Dark Matter

Pseudoscalars (Axions): φ → -φ

→ Time-varying spin-

dependent effects

P

QCD axion resolves strong CP problem

1000-fold improvement

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SLIDE 38

“Axion Wind” Spin-Precession Effect

[Flambaum, talk at Patras Workshop, 2013], [Graham, Rajendran, PRD 88, 035023 (2013)], [Stadnik, Flambaum, PRD 89, 043522 (2014)]

Pseudo-magnetic field *

* Compare with usual magnetic field: H = -µf ·B

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SLIDE 39

Oscillating Electric Dipole Moments

Electric Dipole Moment (EDM) = parity (P) and time- reversal-invariance (T) violating electric moment

Nucleons: [Graham, Rajendran, PRD 84, 055013 (2011)] Atoms and molecules: [Stadnik, Flambaum, PRD 89, 043522 (2014)]

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SLIDE 40

Searching for Spin-Dependent Effects

Use spin-polarised sources: Atomic magnetometers, ultracold neutrons, torsion pendula

Proposals: [Flambaum, talk at Patras Workshop, 2013; Stadnik, Flambaum, PRD 89, 043522 (2014); arXiv:1511.04098; Stadnik, PhD Thesis (2017)]

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SLIDE 41

Searching for Spin-Dependent Effects

Use spin-polarised sources: Atomic magnetometers, ultracold neutrons, torsion pendula

Proposals: [Flambaum, talk at Patras Workshop, 2013; Stadnik, Flambaum, PRD 89, 043522 (2014); arXiv:1511.04098; Stadnik, PhD Thesis (2017)] Experiment (n/Hg): [nEDM collaboration, PRX 7, 041034 (2017)]

B-field effect Axion DM effect

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SLIDE 42

Searching for Spin-Dependent Effects

Use spin-polarised sources: Atomic magnetometers, ultracold neutrons, torsion pendula

Proposals: [Flambaum, talk at Patras Workshop, 2013; Stadnik, Flambaum, PRD 89, 043522 (2014); arXiv:1511.04098; Stadnik, PhD Thesis (2017)]

B-field effect Axion DM effect

Experiment (n/Hg): [nEDM collaboration, PRX 7, 041034 (2017)]

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SLIDE 43

Searching for Spin-Dependent Effects

Use spin-polarised sources: Atomic magnetometers, ultracold neutrons, torsion pendula

σ E B

Proposals: [Flambaum, talk at Patras Workshop, 2013; Stadnik, Flambaum, PRD 89, 043522 (2014); arXiv:1511.04098; Stadnik, PhD Thesis (2017)] Experiment (n/Hg): [nEDM collaboration, PRX 7, 041034 (2017)]

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Searching for Spin-Dependent Effects

Use spin-polarised sources: Atomic magnetometers, ultracold neutrons, torsion pendula

Earth’s rotation

σ E B

Proposals: [Flambaum, talk at Patras Workshop, 2013; Stadnik, Flambaum, PRD 89, 043522 (2014); arXiv:1511.04098; Stadnik, PhD Thesis (2017)]

Beff

Experiment (n/Hg): [nEDM collaboration, PRX 7, 041034 (2017)]

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SLIDE 45

Searching for Spin-Dependent Effects

Use nuclear magnetic resonance (“sidebands” technique)

Proposals: [CASPEr collaboration, Quantum Sci. Technol. 3, 014008 (2018)]

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SLIDE 46

Searching for Spin-Dependent Effects

Use nuclear magnetic resonance (“sidebands” technique)

Proposals: [CASPEr collaboration, Quantum Sci. Technol. 3, 014008 (2018)] Experiment (Formic acid): [CASPEr collaboration, In preparation]

HJ ~ J IH·IC

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SLIDE 47

Searching for Spin-Dependent Effects

Use nuclear magnetic resonance (“sidebands” technique)

Proposals: [CASPEr collaboration, Quantum Sci. Technol. 3, 014008 (2018)] Experiment (Formic acid): [CASPEr collaboration, In preparation]

HJ ~ J IH·IC

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SLIDE 48

Searching for Spin-Dependent Effects

Use nuclear magnetic resonance (“sidebands” technique)

Proposals: [CASPEr collaboration, Quantum Sci. Technol. 3, 014008 (2018)] Experiment (Formic acid): [CASPEr collaboration, In preparation]

HJ ~ J IH·IC

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SLIDE 49

Searching for Spin-Dependent Effects

Use nuclear magnetic resonance (“sidebands” technique)

Proposals: [CASPEr collaboration, Quantum Sci. Technol. 3, 014008 (2018)] Experiment (Formic acid): [CASPEr collaboration, In preparation]

HJ ~ J IH·IC

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SLIDE 50

Searching for Spin-Dependent Effects

Proposals: [Budker, Graham, Ledbetter, Rajendran, A. O. Sushkov, PRX 4, 021030 (2014)]

Use nuclear magnetic resonance

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SLIDE 51

Searching for Spin-Dependent Effects

Proposals: [Budker, Graham, Ledbetter, Rajendran, A. O. Sushkov, PRX 4, 021030 (2014)]

Resonance: 2µBext = ω

Traditional NMR

Use nuclear magnetic resonance

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SLIDE 52

Searching for Spin-Dependent Effects

Proposals: [Budker, Graham, Ledbetter, Rajendran, A. O. Sushkov, PRX 4, 021030 (2014)]

Resonance: 2µBext = ω Resonance: 2µBext ≈ ma

Traditional NMR Dark-matter-driven NMR Measure transverse magnetisation

Use nuclear magnetic resonance

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SLIDE 53

nEDM constraints: [nEDM collaboration, PRX 7, 041034 (2017)] 3 orders of magnitude improvement!

Constraints on Interaction of Axion Dark Matter with Gluons

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SLIDE 54

Constraints on Interaction of Axion Dark Matter with Nucleons

νn/νHg constraints: [nEDM collaboration, PRX 7, 041034 (2017)] 40-fold improvement (laboratory bounds)!

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SLIDE 55

Constraints on Interaction of Axion Dark Matter with Nucleons

νn/νHg constraints: [nEDM collaboration, PRX 7, 041034 (2017)]

Expected sensitivity (atomic co-magnetometry)

40-fold improvement (laboratory bounds)!

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SLIDE 56

Constraints on Interaction of Axion Dark Matter with Nucleons

νn/νHg constraints: [nEDM collaboration, PRX 7, 041034 (2017)] 2 orders of magnitude improvement (laboratory bounds)! Formic acid NMR constraints: [CASPEr collaboration, In preparation]

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SLIDE 57

Summary

  • New classes of dark matter effects that are

first power in the underlying interaction constant => Up to 15 orders of magnitude improvement

  • Improved limits on dark bosons from atomic

experiments (new forces, independent of ρDM)

  • More details in full slides (also on ResearchGate)