1 / 38

Yevgeny Stadnik

Yevgeny Stadnik. New Atomic Probes for Dark Matter and Neutrino-Mediated Forces. Humboldt Fellow. Johannes Gutenberg University, Mainz, Germany. Collaborators (Theory): Victor Flambaum. Collaborators (Experiment): nEDM collaboration at PSI and Sussex

crystalburnett
Download Presentation

Yevgeny Stadnik

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Yevgeny Stadnik New Atomic Probes for Dark Matter and Neutrino-Mediated Forces Humboldt Fellow Johannes Gutenberg University, Mainz, Germany Collaborators (Theory): Victor Flambaum Collaborators (Experiment): nEDM collaboration at PSI and Sussex BASE collaboration at CERN and RIKEN CASPEr collaboration at Mainz PSAS, Vienna, May 2018

  2. Motivation 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

  3. Motivation Traditional “scattering-off-nuclei” searches for heavy WIMP dark matter particles (mχ ~ GeV) have not yet produced a strong positive result.

  4. Motivation Traditional “scattering-off-nuclei” searches for heavy WIMP dark matter particles (mχ ~ GeV) have not yet produced a strong positive result.

  5. Motivation Traditional “scattering-off-nuclei” searches for heavy WIMP dark matter particles (mχ ~ GeV) have not yet produced a strong positive result.

  6. 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 powerin a small interaction constant (eי << 1)!

  7. 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 powerin the interaction constant?

  8. Low-Mass Spin-0 Dark Matter • Low-mass spin-0 particles form a coherently oscillating classicalfield φ(t) = φ0 cos(mφc2t/ℏ), with energy density <ρφ>≈ mφ2φ02/2 (ρDM,local≈ 0.4 GeV/cm3)

  9. Low-Mass Spin-0 Dark Matter • Low-mass spin-0 particles form a coherently oscillating classicalfield φ(t) = φ0 cos(mφc2t/ℏ), with energy density <ρφ>≈ mφ2φ02/2 (ρDM,local≈ 0.4 GeV/cm3) • Coherently oscillating field, since cold (Eφ≈mφc2)

  10. Low-Mass Spin-0 Dark Matter • Low-mass spin-0 particles form a coherently oscillating classicalfield φ(t) = φ0 cos(mφc2t/ℏ), with energy density <ρφ>≈ mφ2φ02/2 (ρDM,local≈ 0.4 GeV/cm3) • Coherently oscillating field, since cold (Eφ≈mφc2) • Classical field for mφ≲ 0.1 eV, sincenφ(λdB,φ/2π)3 >> 1

  11. Low-Mass Spin-0 Dark Matter • Low-mass spin-0 particles form a coherently oscillating classicalfield φ(t) = φ0 cos(mφc2t/ℏ), with energy density <ρφ>≈ mφ2φ02/2 (ρDM,local≈ 0.4 GeV/cm3) • Coherently oscillating field, since cold (Eφ≈mφc2) • Classical field for mφ≲ 0.1 eV, sincenφ(λdB,φ/2π)3 >> 1 • Coherent + classical DM field = “Cosmic laser field”

  12. Low-Mass Spin-0 Dark Matter • Low-mass spin-0 particles form a coherently oscillating classicalfield φ(t) = φ0 cos(mφc2t/ℏ), with energy density <ρφ>≈ mφ2φ02/2 (ρDM,local≈ 0.4 GeV/cm3) • Coherently oscillating field, since cold (Eφ≈mφc2) • Classical field for mφ≲ 0.1 eV, sincenφ(λdB,φ/2π)3 >> 1 • Coherent + classical DM field = “Cosmic laser field” • 10-22eV≲mφ≲ 0.1 eV <=> 10-8 Hz ≲f≲ 1013 Hz λdB,φ≤ Ldwarf galaxy~ 1 kpc Classical field

  13. Low-Mass Spin-0 Dark Matter • Low-mass spin-0 particles form a coherently oscillating classicalfield φ(t) = φ0 cos(mφc2t/ℏ), with energy density <ρφ>≈ mφ2φ02/2 (ρDM,local≈ 0.4 GeV/cm3) • Coherently oscillating field, since cold (Eφ≈mφc2) • Classical field for mφ≲ 0.1 eV, sincenφ(λdB,φ/2π)3 >> 1 • Coherent + classical DM field = “Cosmic laser field” • 10-22eV≲mφ≲ 0.1 eV <=> 10-8 Hz ≲f≲ 1013 Hz • mφ ~ 10-22eV <=> T ~ 1 year λdB,φ≤ Ldwarf galaxy~ 1 kpc Classical field

  14. Low-Mass Spin-0 Dark Matter • Low-mass spin-0 particles form a coherently oscillating classicalfield φ(t) = φ0 cos(mφc2t/ℏ), with energy density <ρφ>≈ mφ2φ02/2 (ρDM,local≈ 0.4 GeV/cm3)

  15. Low-Mass Spin-0 Dark Matter • Low-mass spin-0 particles form a coherently oscillating classicalfield φ(t) = φ0 cos(mφc2t/ℏ), with energy density <ρφ>≈ mφ2φ02/2 (ρDM,local≈ 0.4 GeV/cm3) • 10-22eV≲mφ≲ 0.1 eV inaccessible to traditional “scattering-off-nuclei” searches, since |pφ| ~ 10-3mφ is extremely small => recoil effects of individual particles suppressed

  16. Low-Mass Spin-0 Dark Matter • Low-mass spin-0 particles form a coherently oscillating classicalfield φ(t) = φ0 cos(mφc2t/ℏ), with energy density <ρφ>≈ mφ2φ02/2 (ρDM,local≈ 0.4 GeV/cm3) • 10-22eV≲mφ≲ 0.1 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 fieldin low-energy atomic and astrophysical phenomena that are first power in the interaction constant κ:

  17. Low-Mass Spin-0 Dark Matter • Low-mass spin-0 particles form a coherently oscillating classicalfield φ(t) = φ0 cos(mφc2t/ℏ), with energy density <ρφ>≈ mφ2φ02/2 (ρDM,local≈ 0.4 GeV/cm3) • 10-22eV≲mφ≲ 0.1 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 fieldin 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(!)

  18. Low-Mass Spin-0 Dark Matter Dark Matter Scalars (Dilatons): φ→ +φ Pseudoscalars (Axions): φ→ -φ P P → Time-varying fundamental constants → Time-varying spin-dependent effects 1015-fold improvement 1000-fold improvement

  19. Low-Mass Spin-0 Dark Matter Dark Matter Pseudoscalars (Axions): φ→ -φ QCD axion resolves strong CP problem P → Time-varying spin-dependent effects 1000-fold improvement

  20. “Axion Wind” Spin-Precession Effect [Flambaum, talk at Patras Workshop, 2013], [Graham, Rajendran, PRD88, 035023 (2013)], [Stadnik, Flambaum, PRD89, 043522 (2014)] Pseudo-magnetic field

  21. Oscillating Electric Dipole Moments Nucleons: [Graham, Rajendran, PRD84, 055013 (2011)] Atoms and molecules: [Stadnik, Flambaum, PRD89, 043522 (2014)] Electric Dipole Moment (EDM) = parity (P) and time-reversal-invariance (T) violating electric moment

  22. Searching for Spin-Dependent Effects Proposals:[Flambaum, talk at Patras Workshop, 2013; Stadnik, Flambaum, PRD89, 043522 (2014); arXiv:1511.04098; Stadnik, PhD Thesis (2017)] Use spin-polarised sources: Atomic magnetometers, ultracold neutrons, torsion pendula

  23. Searching for Spin-Dependent Effects Proposals:[Flambaum, talk at Patras Workshop, 2013; Stadnik, Flambaum, PRD89, 043522 (2014); arXiv:1511.04098; Stadnik, PhD Thesis (2017)] Use spin-polarised sources: Atomic magnetometers, ultracold neutrons, torsion pendula Experiment (n/Hg):[nEDM collaboration, PRX7, 041034 (2017)] B-field effect Axion DM effect

  24. Searching for Spin-Dependent Effects Proposals:[Flambaum, talk at Patras Workshop, 2013; Stadnik, Flambaum, PRD89, 043522 (2014); arXiv:1511.04098; Stadnik, PhD Thesis (2017)] Use spin-polarised sources: Atomic magnetometers, ultracold neutrons, torsion pendula Experiment (n/Hg):[nEDM collaboration, PRX7, 041034 (2017)] B-field effect Axion DM effect

  25. Searching for Spin-Dependent Effects Proposals:[Flambaum, talk at Patras Workshop, 2013; Stadnik, Flambaum, PRD89, 043522 (2014); arXiv:1511.04098; Stadnik, PhD Thesis (2017)] Use spin-polarised sources: Atomic magnetometers, ultracold neutrons, torsion pendula Experiment (n/Hg):[nEDM collaboration, PRX7, 041034 (2017)] E σ B

  26. Searching for Spin-Dependent Effects Proposals:[Flambaum, talk at Patras Workshop, 2013; Stadnik, Flambaum, PRD89, 043522 (2014); arXiv:1511.04098; Stadnik, PhD Thesis (2017)] Use spin-polarised sources: Atomic magnetometers, ultracold neutrons, torsion pendula Experiment (n/Hg):[nEDM collaboration, PRX7, 041034 (2017)] E σ B Beff Earth’s rotation

  27. Constraints on Interaction of Axion Dark Matter with Gluons nEDM constraints: [nEDM collaboration, PRX7, 041034 (2017)] 3 orders of magnitude improvement!

  28. Constraints on Interaction of Axion Dark Matter with Nucleons νn/νHg constraints: [nEDM collaboration, PRX7, 041034 (2017)] 40-fold improvement (laboratory bounds)!

  29. Constraints on Interaction of Axion Dark Matter with Nucleons νn/νHg constraints: [nEDM collaboration, PRX7, 041034 (2017)] 40-fold improvement (laboratory bounds)! Expected sensitivity (atomic co-magnetometry)

  30. Classical (Tree-Level) Weak Force [r >> 1/mZ]

  31. “Long-Range” Neutrino-Mediated Forces [1/mZ,W << r << 1/(2mν)]

  32. Probing “Long-Range” Neutrino-Mediated Forces [Stadnik, arXiv:1711.03700, PRL (In press)]

  33. Probing “Long-Range” Neutrino-Mediated Forces [Stadnik, arXiv:1711.03700, PRL (In press)] Enormous enhancement of energy shift in s-wave atomic states (l = 0, no centrifugal barrier)!

  34. Probing “Long-Range” Neutrino-Mediated Forces [Stadnik, arXiv:1711.03700, PRL (In press)] Enormous enhancement of energy shift in s-wave atomic states (l = 0, no centrifugal barrier)! rc = “cutoff” radius Finite-sized nucleus: (aB/rc)2 ≈ (aB/Rnucl)2 ~ 109 Point-like nucleus: (aB/rc)2 ≈ (aB/λZ,W)2 ~ 1015

  35. Probing “Long-Range” Neutrino-Mediated Forces [Stadnik, arXiv:1711.03700, PRL (In press)] • Spectroscopy measurements of and calculations in: • Simple atoms (H, D) • Exotic atoms (e-e+, e-μ+) • Simple nuclei (np) • Heavy atoms (Ca+)

  36. Probing “Long-Range” Neutrino-Mediated Forces [Stadnik, arXiv:1711.03700, PRL (In press)] • Spectroscopy measurements of and calculations in: • Simple atoms (H, D) • Exotic atoms (e-e+, e-μ+) • Simple nuclei (np) • Heavy atoms (Ca+) Muonium ground-state hyperfine interval: Δνneutrinos ≈ 0.5 Hz νexp = 4463302776(51) Hz νtheor = 4463302868(271)* Hz Δνneutrinos + other fermions ≈ 2 Hz *u[νtheor(me/mμ)] ≈ 260 Hz, u[νtheor(4th-order QED)] ≈ 85 Hz, u[νtheor(others)] ≲ Hz

  37. Constraints on “Long-Range” Neutrino-Mediated Forces [Stadnik, arXiv:1711.03700, PRL (In press)] 18 orders of magnitude improvement!

  38. 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 (independent of ρDM) • 18 orders of magnitude improvement on “long-range” neutrino-mediated forces from atomic spectroscopy (Can we test the SM prediction?) • More details in full slides (also on ResearchGate)

More Related