Manifestations of Low-Mass Dark Bosons

Transcription

1 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 at PSI and Sussex BASE collaboration at CERN and RIKEN Beyond Standard Model: Where do we go from here?, Florence, September 2018

2 Motivation for Low-Mass Dark Bosons Low-mass (m << 100 GeV) dark bosons may explain several outstanding puzzles

3 Dark Matter Overwhelming astrophysical evidence for existence of dark matter (~5 times more dark matter than ordinary matter). ρ DM 0.4 GeV/cm 3 v DM ~ 300 km/s

4 Motivation for Low-Mass Dark Bosons 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

5 Manifestations of Dark Bosons New forces Stellar emission Interconversion with ordinary particles Dark matter

6 Manifestations of Dark Bosons New forces Stellar emission Interconversion with ordinary particles Dark matter

7 Manifestations of Dark Bosons New forces Stellar emission Interconversion with ordinary particles Dark matter

8 Basics of Atomic EDMs Electric Dipole Moment (EDM) = parity (P) and time-reversalinvariance (T) violating electric moment

9 Basics of Atomic EDMs Electric Dipole Moment (EDM) = parity (P) and time-reversalinvariance (T) violating electric moment

10 Basics of Atomic EDMs Electric Dipole Moment (EDM) = parity (P) and time-reversalinvariance (T) violating electric moment

11 Sensitivity of EDM Experiments d Hg limit 7*10-30 e cm

12 Sensitivity of EDM Experiments d Hg limit 7*10-30 e cm +δq (d Hg ) classical = δq L Hg L Hg 3*10-8 cm -δq

13 Sensitivity of EDM Experiments d Hg limit 7*10-30 e cm +δq (d Hg ) classical = δq L Hg L Hg 3*10-8 cm -δq δq sensitivity ~ e (!)

14 Non-Cosmological Sources of Dark Bosons [Stadnik, Dzuba, Flambaum, PRL 120, (2018)], [Dzuba, Flambaum, Samsonov, Stadnik, PRD 98, (2018)]

15 Non-Cosmological Sources of Dark Bosons [Stadnik, Dzuba, Flambaum, PRL 120, (2018)], [Dzuba, Flambaum, Samsonov, Stadnik, PRD 98, (2018)] P,T-violating forces => Atomic and Molecular EDMs

16 Non-Cosmological Sources of Dark Bosons [Stadnik, Dzuba, Flambaum, PRL 120, (2018)], [Dzuba, Flambaum, Samsonov, Stadnik, PRD 98, (2018)] P,T-violating forces => Atomic and Molecular EDMs Atomic EDM experiments: Cs, Tl, Xe, Hg, Ra Molecular EDM experiments: YbF, HfF +, ThO

17 Constraints on Scalar-Pseudoscalar Electron-Electron Interaction EDM constraints: [Stadnik, Dzuba, Flambaum, PRL 120, (2018)] Many orders of magnitude improvement!

18 Manifestations of Dark Bosons New forces Stellar emission Interconversion with ordinary particles Dark matter

19 Motivation Traditional scattering-off-nuclei searches for heavy WIMP dark matter particles (m χ ~ GeV) have not yet produced a strong positive result.

20 Motivation Traditional scattering-off-nuclei searches for heavy WIMP dark matter particles (m χ ~ GeV) have not yet produced a strong positive result.

21 Motivation Traditional scattering-off-nuclei searches for heavy WIMP dark matter particles (m χ ~ GeV) have not yet produced a strong positive result.

22 Motivation Traditional scattering-off-nuclei searches for heavy WIMP dark matter particles (m χ ~ GeV) have not yet produced a strong positive result. Challenge: Observable is fourth power in a small 1)! << יe ) interaction constant

23 Motivation Traditional scattering-off-nuclei searches for heavy WIMP dark matter particles (m χ ~ 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?

24 Low-mass Spin-0 Dark Matter Low-mass spin-0 particles form a coherently oscillating classical field φ(t) = φ 0 cos(m φ c 2 t/ħ), with energy density <ρ φ > m φ 2 φ 02 /2 (ρ DM,local 0.4 GeV/cm 3 )

25 Low-mass Spin-0 Dark Matter Low-mass spin-0 particles form a coherently oscillating classical field φ(t) = φ 0 cos(m φ c 2 t/ħ), with energy density <ρ φ > m φ 2 φ 02 /2 (ρ DM,local 0.4 GeV/cm 3 )

26 Low-mass Spin-0 Dark Matter Low-mass spin-0 particles form a coherently oscillating classical field φ(t) = φ 0 cos(m φ c 2 t/ħ), with energy density <ρ φ > m φ 2 φ 02 /2 (ρ DM,local 0.4 GeV/cm 3 ) H >> m φ : φ const. => ρ const. [Dark energy regime]

27 Low-mass Spin-0 Dark Matter Low-mass spin-0 particles form a coherently oscillating classical field φ(t) = φ 0 cos(m φ c 2 t/ħ), with energy density <ρ φ > m φ 2 φ 02 /2 (ρ DM,local 0.4 GeV/cm 3 ) H >> m φ : φ const. => ρ const. [Dark energy regime] H << m φ : φ cos(m φ t)/t 3/4 => ρ 1/V [Cold DM regime]

28 Low-mass Spin-0 Dark Matter Low-mass spin-0 particles form a coherently oscillating classical field φ(t) = φ 0 cos(m φ c 2 t/ħ), with energy density <ρ φ > m φ 2 φ 02 /2 (ρ DM,local 0.4 GeV/cm 3 ) Coherently oscillating field, since cold (E φ m φ c 2 )

29 Low-mass Spin-0 Dark Matter Low-mass spin-0 particles form a coherently oscillating classical field φ(t) = φ 0 cos(m φ c 2 t/ħ), with energy density <ρ φ > m φ 2 φ 02 /2 (ρ DM,local 0.4 GeV/cm 3 ) Coherently oscillating field, since cold (E φ m φ c 2 ) Classical field for m φ << 1 ev, since n φ (λ db,φ /2π) 3 >> 1

30 Low-mass Spin-0 Dark Matter Low-mass spin-0 particles form a coherently oscillating classical field φ(t) = φ 0 cos(m φ c 2 t/ħ), with energy density <ρ φ > m φ 2 φ 02 /2 (ρ DM,local 0.4 GeV/cm 3 ) Coherently oscillating field, since cold (E φ m φ c 2 ) Classical field for m φ << 1 ev, since n φ (λ db,φ /2π) 3 >> 1 Coherent + classical DM field = Cosmic laser field

31 Low-mass Spin-0 Dark Matter Low-mass spin-0 particles form a coherently oscillating classical field φ(t) = φ 0 cos(m φ c 2 t/ħ), with energy density <ρ φ > m φ 2 φ 02 /2 (ρ DM,local 0.4 GeV/cm 3 ) Coherently oscillating field, since cold (E φ m φ c 2 ) Classical field for m φ << 1 ev, since n φ (λ db,φ /2π) 3 >> 1 Coherent + classical DM field = Cosmic laser field ev m φ << 1 ev <=> 10-8 Hz f << Hz λ db,φ L dwarf galaxy ~ 1 kpc Classical field

32 Low-mass Spin-0 Dark Matter Low-mass spin-0 particles form a coherently oscillating classical field φ(t) = φ 0 cos(m φ c 2 t/ħ), with energy density <ρ φ > m φ 2 φ 02 /2 (ρ DM,local 0.4 GeV/cm 3 ) Coherently oscillating field, since cold (E φ m φ c 2 ) Classical field for m φ << 1 ev, since n φ (λ db,φ /2π) 3 >> 1 Coherent + classical DM field = Cosmic laser field ev m φ << 1 ev <=> 10-8 Hz f << Hz λ db,φ L dwarf galaxy ~ 1 kpc Classical field m φ ~ ev <=> T ~ 1 year

33 Low-mass Spin-0 Dark Matter Low-mass spin-0 particles form a coherently oscillating classical field φ(t) = φ 0 cos(m φ c 2 t/ħ), with energy density <ρ φ > m φ2 φ 02 /2 (ρ DM,local 0.4 GeV/cm 3 )

34 Low-mass Spin-0 Dark Matter Low-mass spin-0 particles form a coherently oscillating classical field φ(t) = φ 0 cos(m φ c 2 t/ħ), with energy density <ρ φ > m φ2 φ 02 /2 (ρ DM,local 0.4 GeV/cm 3 ) ev m φ << 1 ev inaccessible to traditional scatteringoff-nuclei searches, since p φ ~ 10-3 m φ is extremely small => recoil effects of individual particles suppressed

35 Low-mass Spin-0 Dark Matter Low-mass spin-0 particles form a coherently oscillating classical field φ(t) = φ 0 cos(m φ c 2 t/ħ), with energy density <ρ φ > m φ2 φ 02 /2 (ρ DM,local 0.4 GeV/cm 3 ) ev m φ << 1 ev inaccessible to traditional scatteringoff-nuclei searches, since p φ ~ 10-3 m φ 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 :

36 Low-mass Spin-0 Dark Matter Low-mass spin-0 particles form a coherently oscillating classical field φ(t) = φ 0 cos(m φ c 2 t/ħ), with energy density <ρ φ > m φ2 φ 02 /2 (ρ DM,local 0.4 GeV/cm 3 ) ev m φ << 1 ev inaccessible to traditional scatteringoff-nuclei searches, since p φ ~ 10-3 m φ 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 (!)

37 Low-mass Spin-0 Dark Matter Dark Matter QCD axion resolves strong CP problem Pseudoscalars (Axions): φ P -φ Time-varying spindependent effects 1000-fold improvement

38 Axion Wind Spin-Precession Effect [Flambaum, talk at Patras Workshop, 2013], [Graham, Rajendran, PRD 88, (2013)], [Stadnik, Flambaum, PRD 89, (2014)] Pseudo-magnetic field * * Compare with usual magnetic field: H = -µ f B

39 Oscillating Electric Dipole Moments Nucleons: [Graham, Rajendran, PRD 84, (2011)] Atoms and molecules: [Stadnik, Flambaum, PRD 89, (2014)] Electric Dipole Moment (EDM) = parity (P) and timereversal-invariance (T) violating electric moment

40 Searching for Spin-Dependent Effects Proposals: [Flambaum, talk at Patras Workshop, 2013; Stadnik, Flambaum, 89, (2014); arxiv: ; Stadnik, PhD Thesis (2017)] Use spin-polarised sources: Atomic magnetometers, ultracold neutrons, torsion pendula PRD

41 Searching for Spin-Dependent Effects Proposals: [Flambaum, talk at Patras Workshop, 2013; Stadnik, Flambaum, 89, (2014); arxiv: ; Stadnik, PhD Thesis (2017)] Use spin-polarised sources: Atomic magnetometers, ultracold neutrons, torsion pendula PRD Experiment (n/hg): [nedm collaboration, PRX 7, (2017)] B-field effect Axion DM effect

42 Searching for Spin-Dependent Effects Proposals: [Flambaum, talk at Patras Workshop, 2013; Stadnik, Flambaum, 89, (2014); arxiv: ; Stadnik, PhD Thesis (2017)] Use spin-polarised sources: Atomic magnetometers, ultracold neutrons, torsion pendula PRD Experiment (n/hg): [nedm collaboration, PRX 7, (2017)] B-field effect Axion DM effect

43 Searching for Spin-Dependent Effects Proposals: [Flambaum, talk at Patras Workshop, 2013; Stadnik, Flambaum, 89, (2014); arxiv: ; Stadnik, PhD Thesis (2017)] Use spin-polarised sources: Atomic magnetometers, ultracold neutrons, torsion pendula PRD Experiment (n/hg): [nedm collaboration, PRX 7, (2017)] E σ B

44 Searching for Spin-Dependent Effects Proposals: [Flambaum, talk at Patras Workshop, 2013; Stadnik, Flambaum, 89, (2014); arxiv: ; Stadnik, PhD Thesis (2017)] Use spin-polarised sources: Atomic magnetometers, ultracold neutrons, torsion pendula PRD Experiment (n/hg): [nedm collaboration, PRX 7, (2017)] E σ B B eff Earth s rotation

45 Searching for Spin-Dependent Effects Proposals: [CASPEr collaboration, Quantum Sci. Technol. 3, (2018)] Use nuclear magnetic resonance ( sidebands technique)

46 Searching for Spin-Dependent Effects Proposals: [CASPEr collaboration, Quantum Sci. Technol. 3, (2018)] Use nuclear magnetic resonance ( sidebands technique) Experiment (Formic acid): [CASPEr collaboration, In preparation] H J ~ J I H I C

47 Searching for Spin-Dependent Effects Proposals: [CASPEr collaboration, Quantum Sci. Technol. 3, (2018)] Use nuclear magnetic resonance ( sidebands technique) Experiment (Formic acid): [CASPEr collaboration, In preparation] H J ~ J I H I C

48 Searching for Spin-Dependent Effects Proposals: [CASPEr collaboration, Quantum Sci. Technol. 3, (2018)] Use nuclear magnetic resonance ( sidebands technique) Experiment (Formic acid): [CASPEr collaboration, In preparation] H J ~ J I H I C

49 Searching for Spin-Dependent Effects Proposals: [CASPEr collaboration, Quantum Sci. Technol. 3, (2018)] Use nuclear magnetic resonance ( sidebands technique) Experiment (Formic acid): [CASPEr collaboration, In preparation] H J ~ J I H I C

50 Searching for Spin-Dependent Effects Proposals: [Budker, Graham, Ledbetter, Rajendran, A. O. Sushkov, PRX 4, (2014)] Use nuclear magnetic resonance

51 Searching for Spin-Dependent Effects Proposals: [Budker, Graham, Ledbetter, Rajendran, A. O. Sushkov, PRX 4, (2014)] Use nuclear magnetic resonance Traditional NMR Resonance: 2µB ext = ω

52 Searching for Spin-Dependent Effects Proposals: [Budker, Graham, Ledbetter, Rajendran, A. O. Sushkov, PRX 4, (2014)] Use nuclear magnetic resonance Traditional NMR Dark-matter-driven NMR Resonance: 2µB ext = ω Resonance: 2µB ext m a Measure transverse magnetisation

53 Constraints on Interaction of Axion Dark Matter with Gluons nedm constraints: [nedm collaboration, PRX 7, (2017)] 3 orders of magnitude improvement!

54 Constraints on Interaction of Axion Dark Matter with Nucleons ν n /ν Hg constraints: [nedm collaboration, PRX 7, (2017)] 40-fold improvement (laboratory bounds)!

55 Constraints on Interaction of Axion Dark Matter with Nucleons ν n /ν Hg constraints: [nedm collaboration, PRX 7, (2017)] 40-fold improvement (laboratory bounds)! Expected sensitivity (atomic co-magnetometry)

56 Constraints on Interaction of Axion Dark Matter with Nucleons ν n /ν Hg constraints: [nedm collaboration, PRX 7, (2017)] Formic acid NMR constraints: [CASPEr collaboration, In preparation] 2 orders of magnitude improvement (laboratory bounds)!

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 ρ DM ) More details in full slides (also on ResearchGate)