Manifestations of Low-Mass Dark Bosons · 2018-09-05 · [Stadnik, Dzuba, Flambaum, PRL 120, 013202...
Transcript of Manifestations of Low-Mass Dark Bosons · 2018-09-05 · [Stadnik, Dzuba, Flambaum, PRL 120, 013202...
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Yevgeny StadnikHumboldt 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
of dark matter (~5 times more dark matter than ordinary matter).
ρDM ≈ 0.4 GeV/cm3
vDM ~ 300 km/s
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“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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Manifestations of Dark Bosons
New forces
Interconversion with ordinary particles
Stellar emission
Dark matter
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Manifestations of Dark Bosons
New forces
Interconversion with ordinary particles
Stellar emission
Dark matter
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Manifestations of Dark Bosons
New forces
Interconversion with ordinary particles
Stellar emission
Dark matter
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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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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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|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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[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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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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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 ordinary particles
Stellar emission
Dark matter
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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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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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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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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 (e1 >> י)!
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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> ≈ mφ2φ0
2/2 (ρDM,local ≈ 0.4 GeV/cm3)
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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> ≈ mφ2φ0
2/2 (ρDM,local ≈ 0.4 GeV/cm3)
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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> ≈ mφ2φ0
2/2 (ρDM,local ≈ 0.4 GeV/cm3)
H >> mφ: φ ≈ const. => ρ ≈ const. [Dark energy 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> ≈ mφ2φ0
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> ≈ mφ2φ0
2/2 (ρDM,local ≈ 0.4 GeV/cm3)
• Coherently oscillating field, since cold (Eφ ≈ mφc2)
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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> ≈ mφ2φ0
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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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> ≈ mφ2φ0
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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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> ≈ mφ2φ0
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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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> ≈ mφ2φ0
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 yearλdB,φ ≤ L dwarf galaxy ~ 1 kpc Classical field
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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>
≈ mφ2φ0
2/2 (ρDM,local ≈ 0.4 GeV/cm3)
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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>
≈ mφ2φ0
2/2 (ρDM,local ≈ 0.4 GeV/cm3)
• 10-22 eV ≲ mφ << 1 eV inaccessible to traditional “scattering-off-nuclei” searches, since |pφ| ~ 10-3mφ is extremely small => recoil effects of individual particles suppressed
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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>
≈ mφ2φ0
2/2 (ρDM,local ≈ 0.4 GeV/cm3)
• 10-22 eV ≲ mφ << 1 eV inaccessible to traditional “scattering-off-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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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>
≈ mφ2φ0
2/2 (ρDM,local ≈ 0.4 GeV/cm3)
• 10-22 eV ≲ mφ << 1 eV inaccessible to traditional “scattering-off-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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Low-mass Spin-0 Dark MatterDark Matter
Pseudoscalars (Axions): φ → -φ
→ Time-varying spin-dependent effects
P
QCD axion resolves strong CP problem
1000-fold improvement
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“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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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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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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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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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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Searching for Spin-Dependent Effects
Use spin-polarised sources: Atomic magnetometers, ultracold neutrons, torsion pendula
σE 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
σE 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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Searching for Spin-Dependent Effects
Use nuclear magnetic resonance (“sidebands” technique)Proposals: [CASPEr collaboration, Quantum Sci. Technol. 3, 014008 (2018)]
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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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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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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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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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Searching for Spin-Dependent EffectsProposals: [Budker, Graham, Ledbetter, Rajendran, A. O. Sushkov, PRX 4, 021030 (2014)]
Use nuclear magnetic resonance
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Searching for Spin-Dependent EffectsProposals: [Budker, Graham, Ledbetter, Rajendran, A. O. Sushkov, PRX 4, 021030 (2014)]
Resonance: 2µBext = ω
Traditional NMR
Use nuclear magnetic resonance
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Searching for Spin-Dependent EffectsProposals: [Budker, Graham, Ledbetter, Rajendran, A. O. Sushkov, PRX 4, 021030 (2014)]
Resonance: 2µBext = ωResonance: 2µBext ≈ ma
Traditional NMR Dark-matter-driven NMR
Measure transverse magnetisation
Use nuclear magnetic resonance
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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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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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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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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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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)