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Low-Energy Atomic Probes of Dark Bosons and Neutrino-Mediated Forces

Explore manifestations of dark bosons, new forces, and interactions with ordinary particles through atomic spectroscopy and EDM measurements. Collaborate with experts to delve into the realm of dark matter.

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Low-Energy Atomic Probes of Dark Bosons and Neutrino-Mediated Forces

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  1. Yevgeny Stadnik Low-Energy Atomic Probes of Dark Bosons 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 MITP Scientific Program, Mainz, May 2018

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

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

  4. Manifestations of Dark Bosons New forces Atomic spectroscopy: Leefer, Gerhardus, Budker, Flambaum, Stadnik, PRL117, 271601 (2016) Ficek, Fadeev, Flambaum, Kimball, Kozlov, Stadnik, Budker, 1801.00491, PRL (In press) Atomic PNC: Dzuba, Flambaum, Stadnik, PRL119, 223201 (2017) Atomic and molecular EDMs: Stadnik, Dzuba, Flambaum, PRL120, 013202 (2018)

  5. Manifestations of Dark Bosons New forces Atomic spectroscopy: Leefer, Gerhardus, Budker, Flambaum, Stadnik, PRL117, 271601 (2016) Ficek, Fadeev, Flambaum, Kimball, Kozlov, Stadnik, Budker, 1801.00491, PRL (In press) Atomic PNC: Dzuba, Flambaum, Stadnik, PRL119, 223201 (2017) Atomic and molecular EDMs: Stadnik, Dzuba, Flambaum, PRL120, 013202 (2018)

  6. Basics of Atomic PNC Parity violation in weak neutral current interactions first discovered in bismuth optical rotation experiments in Novosibirsk [Barkov, Zolotorev, JETP Lett.27, 357 (1978); Pis’ma Zh. Eksp. Teor. Fiz.27, 379 (1978)]

  7. Basics of Atomic PNC Parity violation in weak neutral current interactions first discovered in bismuth optical rotation experiments in Novosibirsk [Barkov, Zolotorev, JETP Lett.27, 357 (1978); Pis’ma Zh. Eksp. Teor. Fiz.27, 379 (1978)] – +

  8. Basics of Atomic PNC Parity violation in weak neutral current interactions first discovered in bismuth optical rotation experiments in Novosibirsk [Barkov, Zolotorev, JETP Lett.27, 357 (1978); Pis’ma Zh. Eksp. Teor. Fiz.27, 379 (1978)] – + QW (133Cs) = -72.58(29)exp(32)theory c.f. QW (133Cs)SM = -73.23(2) Experiment:[Wood et al., Science275, 1759 (1997)] Theory:[Dzuba, Berengut, Flambaum, Roberts, PRL109, 203003 (2012)]

  9. Basics of Atomic PNC • Atomic PNC dominated by Z-boson exchange between valence electron and the nucleus at distance r ~ Rnucl (equivalently momentum transfer q ~ 1/Rnucl >> me)

  10. Basics of Atomic PNC • Atomic PNC dominated by Z-boson exchange between valence electron and the nucleus at distance r ~ Rnucl (equivalently momentum transfer q ~ 1/Rnucl >> me) • Bound-state valence electron (|Ebind| << me) has definite energy: E ≈ me

  11. Basics of Atomic PNC • Atomic PNC dominated by Z-boson exchange between valence electron and the nucleus at distance r ~ Rnucl (equivalently momentum transfer q ~ 1/Rnucl >> me) • Bound-state valence electron (|Ebind| << me) has definite energy: E ≈ me • BUT indefinite momentum!

  12. Basics of Atomic PNC • Atomic PNC dominated by Z-boson exchange between valence electron and the nucleus at distance r ~ Rnucl (equivalently momentum transfer q ~ 1/Rnucl >> me) • Bound-state valence electron (|Ebind| << me) has definite energy: E ≈ me • BUT indefinite momentum! • At r ~ Rnucl, |p|2 >> E2 ≈ me2 => Highly off-mass-shell electron!

  13. Basics of Atomic PNC • Atomic PNC dominated by Z-boson exchange between valence electron and the nucleus at distance r ~ Rnucl (equivalently momentum transfer q ~ 1/Rnucl >> me) • Bound-state valence electron (|Ebind| << me) has definite energy: E ≈ me • BUT indefinite momentum! • At r ~ Rnucl, |p|2 >> E2 ≈ me2 => Highly off-mass-shell electron! • Example: <ns1/2|Hweak|n′p1/2> in Cs

  14. Basics of Atomic PNC • Atomic PNC dominated by Z-boson exchange between valence electron and the nucleus at distance r ~ Rnucl (equivalently momentum transfer q ~ 1/Rnucl >> me) • Bound-state valence electron (|Ebind| << me) has definite energy: E ≈ me • BUT indefinite momentum! • At r ~ Rnucl, |p|2 >> E2 ≈ me2 => Highly off-mass-shell electron! • Example: <ns1/2|Hweak|n′p1/2> in Cs • If qtypical ~ 1/Rnucl >> me, then Krel ≈ 3 [Bouchiat, Bouchiat, J. de Phys.35, 899 (1974)]

  15. Basics of Atomic PNC • Atomic PNC dominated by Z-boson exchange between valence electron and the nucleus at distance r ~ Rnucl (equivalently momentum transfer q ~ 1/Rnucl >> me) • Bound-state valence electron (|Ebind| << me) has definite energy: E ≈ me • BUT indefinite momentum! • At r ~ Rnucl, |p|2 >> E2 ≈ me2 => Highly off-mass-shell electron! • Example: <ns1/2|Hweak|n′p1/2> in Cs • If qtypical ~ 1/Rnucl >> me, then Krel ≈ 3 • If qtypical<< me (like, e.g., in Z-boson exchange between valence electron and 1s electrons), then Krel ≈ 1 [Bouchiat, Bouchiat, J. de Phys.35, 899 (1974)]

  16. Basics of Atomic EDMs Electric Dipole Moment (EDM) = parity (P) and time-reversal-invariance (T) violating electric moment

  17. Basics of Atomic EDMs Electric Dipole Moment (EDM) = parity (P) and time-reversal-invariance (T) violating electric moment

  18. Non-Cosmological Sources of Dark Bosons [Dzuba, Flambaum, Stadnik, PRL119, 223201 (2017)]

  19. Non-Cosmological Sources of Dark Bosons [Dzuba, Flambaum, Stadnik, PRL119, 223201 (2017)] P-violating forces => Atomic parity-nonconserving effects and nuclear anapole moments

  20. Non-Cosmological Sources of Dark Bosons [Dzuba, Flambaum, Stadnik, PRL119, 223201 (2017)] P-violating forces => Atomic parity-nonconserving effects and nuclear anapole moments Atomic PNC experiments: Cs, Yb, Tl

  21. Constraints on Vector-Pseudovector Nucleon-Electron Interaction PNC constraints: [Dzuba, Flambaum, Stadnik, PRL119, 223201 (2017)] Many orders of magnitude improvement!

  22. Constraints on Vector-Pseudovector Nucleon-Proton Interaction PNC constraints: [Dzuba, Flambaum, Stadnik, PRL119, 223201 (2017)] Yan, Snow, PRL110, 082003 (2013)

  23. Non-Cosmological Sources of Dark Bosons [Stadnik, Dzuba, Flambaum, PRL120, 013202 (2018)]

  24. Non-Cosmological Sources of Dark Bosons [Stadnik, Dzuba, Flambaum, PRL120, 013202 (2018)] P,T-violating forces => Atomic and Molecular EDMs

  25. Non-Cosmological Sources of Dark Bosons [Stadnik, Dzuba, Flambaum, PRL120, 013202 (2018)] P,T-violating forces => Atomic and Molecular EDMs Atomic EDM experiments: Cs, Tl, Xe, Hg Molecular EDM experiments: YbF, HfF+, ThO

  26. Constraints on Scalar-Pseudoscalar Nucleon-Electron Interaction EDM constraints: [Stadnik, Dzuba, Flambaum, PRL120, 013202 (2018)] Many orders of magnitude improvement!

  27. Constraints on Scalar-Pseudoscalar Electron-Electron Interaction EDM constraints: [Stadnik, Dzuba, Flambaum, PRL120, 013202 (2018)] Many orders of magnitude improvement!

  28. Manifestations of Dark Bosons Dark matter Spectroscopy, interferometry, cavities, BBN, CMB: Stadnik, Flambaum, PRL114, 161301 (2015);PRL115, 201301 (2015); PRA93, 063630 (2016); PRA94, 022111 (2016) Spin-precession effects, EDMs: Stadnik, Flambaum, PRD89, 043522 (2014) nEDM collaboration, PRX7, 041034 (2017)

  29. Manifestations of Dark Bosons Dark matter Spectroscopy, interferometry, cavities, BBN, CMB: Stadnik, Flambaum, PRL114, 161301 (2015);PRL115, 201301 (2015); PRA93, 063630 (2016); PRA94, 022111 (2016) Spin-precession effects, EDMs: Stadnik, Flambaum, PRD89, 043522 (2014) nEDM collaboration, PRX7, 041034 (2017)

  30. 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

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

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

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

  34. 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)!

  35. 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?

  36. 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)

  37. 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)

  38. 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

  39. 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”

  40. 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

  41. 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

  42. 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)

  43. 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

  44. 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:

  45. 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(!)

  46. 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

  47. 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

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

  49. 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

  50. 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

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