Solar Axions Globular Cluster Supernova 1987A Dark Matter Long-Range Force
Axion Landscape
Georg G. Raffelt, Max-Planck-Institut für Physik, München Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 High- and Low-Energy Frontiers in Particle Physics
Cosmological QCD Electroweak GUT Planck constant scale scale scale mass
10−6 10−3 1 103 106 109 1012 1015 1018 1021 1024 1027 eV
Heavy right-handed neutrinos (see-saw mechanism) ퟐ 풎푫 풎푫 푴 푴 WIMP dark matter (related to EW scale, perhaps SUSY)
Axion dark matter (related to Peccei-Quinn symmetry)
풎흅풇흅 풎풂 ∼ 풎흅, 풇흅 풇풂 풇풂
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Bestiarium of Low-Mass Bosons
Weakly Interacting Sub-eV Particles (WISPs)
• Axions (1 parameter family 푚푎푓푎 ∼ 푚휋푓휋) Solves strong CP problem Could be dark matter
• String axions (almost massless pseudoscalars in string theory) One of them may solve CP problem
• Axion-like particles (ALPs) Generic two-photon vertex, could be dark matter (2 parameters 푚푎 and 푔푎훾)
• Hidden photons Low-mass gauge bosons from 푈′(1) (kinetic mixing parameter 휒 and mass 푚훾′)
• Chameleons Scalars in certain models of scalar-tensor gravity Motivated by dark energy Environment-dependent properties
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Plenitude of Axions – Axiverse
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP,[Joerg Mainz 15–19 Jaekel] June 2015 CP Violation in Particle Physics Discrete symmetries in particle physics
C – Charge conjugation, transforms particles to antiparticles violated by weak interactions
P – Parity, changes left-handedness to right-handedness violated by weak interactions
T – Time reversal, changes direction of motion (forward to backward)
CPT – exactly conserved in quantum field theory
CP – conserved by all gauge interactions violated by three-flavor quark mixing matrix All measured CP-violating effects derive from a single phase in the quark mass matrix (Kobayashi-Maskawa phase), i.e. from complex Yukawa couplings
Cosmic matter-antimatter asymmetry requires new ingredients M. Kobayashi T. Maskawa Physics Nobel Prize 2008
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 The CP Problem of Strong Interactions
Real quark Phase from Angle CP-odd mass Yukawa coupling variable quantity ∼ 퐄 ⋅ 퐁 휇휈 훼s 휇휈 ℒ = 휓 i퐷 − 푚 푒i휃푞 휓 − 1 퐺 퐺 − Θ 퐺 퐺 QCD 푞 푞 푞 4 휇휈푎 푎 8휋 휇휈푎 푎 푞 Remove phase of mass term by chiral transformation of quark fields
−푖훾5휃푞/2 휓푞 → 푒 휓푞
훼s ℒ = 휓 i퐷 − 푚 휓 − 1 퐺퐺 − Θ − arg det 푀 퐺퐺 QCD 푞 푞 푞 4 푞 8휋 푞 −휋 ≤Θ≤+휋 Θ can be traded between quark phases and 퐺퐺 term
No physical impact if at least one 푚푞 = 0
Induces a large neutron electric dipole moment (a T-violating quantity)
Experimental limits: 횯 < ퟏퟎ−ퟏퟏ Why so small?
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Strong CP Problem QCD vacuum energy 푉(Θ)
4 ΛQCD Equivalent Equivalent
Θ −2휋 −휋 +휋 +2휋 • CP conserving vacuum has Θ = 0 (Vafa and Witten 1984) • QCD could have any −휋 ≤ Θ ≤ +휋, is “constant of nature” • Energy can not be minimized: Θ not dynamical Peccei-Quinn solution: Make 횯 dynamical, let system relax to lowest energy
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 37 Years of Axions
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 The Cleansing Axion
Frank Wilczek
“I named them after a laundry detergent, since they clean up a problem with an axial current.” (Nobel lecture 2004)
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Phenomenological Axion Properties
Gluon coupling (generic), defines normalization of axion scale 푓푎
훼푠 푎 ℒ푎퐺= 퐺퐺 8휋 푓푎
Mass (generic) depends on up/down quark masses
푚푢푚푑 푚휋 6 휇eV 푚푎 = ≈ 12 푚푢 + 푚푑 푓휋푓푎 푓푎 10 GeV
Axion-photon coupling (model dependent) Generic from 푎-휋-휂 mixing
푔푎훾 훼 퐸 푎 ℒ = − 퐹퐹 푎 = 푔 퐄 ⋅ 퐁 푎 = − 1.92 퐄 ⋅ 퐁 푎훾 4 푎훾 2휋 푁 푓 γ 푎
푎 Model-dependent, γ E/N = 0 (KSVZ), 8/3 (DFSZ), many others
Axion-nucleon coupling (model-dependent numerical factors 퐶푁) 푓 휕휇푎 • Axial-vector current ℒ = 퐶 Ψ 훾휇훾 Ψ 푎 푎푁 푁 푁 5 푁 • Spin-dependent int’n 2푓푎 푓 Axion-electron coupling in non-hadronic models is analogous with 퐶푒
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Axion Bounds and Searches
[GeV] fa 103 106 109 1012 1015
keV eV meV meV neV ma ADMX Search CAST CASPEr Experiments Tele (Seattle & Yale)
scope Hadronic axions
Too much String Too Too much much CDM cold dark matter
hot dark matter DW (re(misalignment)-alignment with Qi = 1)
Future
EUCLID
Helium-burning stars ARIADNE Anthropic (a-g-coupling, hadronic axions) IAXO Range
SN 1987A Too much Too many events energy loss
Globular clusters (He ignition), WD cooling (a-e coupling)
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Let there be light
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Experimental Tests of Invisible Axions
Primakoff effect: Pierre Sikivie:
Axion-photon transition in external Macroscopic B-field can provide a static E or B field large coherent transition rate over (Originally discussed for 휋0 a big volume (low-mass axions)
by Henri Primakoff 1951) • Axion helioscope: Look at the Sun through a dipole magnet
• Axion haloscope: Look for dark-matter axions with a microwave resonant cavity Two-photon vertex generic for 휋0, 휂, axion-like particles (ALPs), gravitons
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Search for Solar Axions Axion Helioscope Primakoff (Sikivie 1983) production N g a Axion flux a g
Magnet S Axion-Photon-Oscillation Sun
Tokyo Axion Helioscope (“Sumico”) (Results since 1998, up again 2008)
CERN Axion Solar Telescope (CAST) (Data since 2003) Alternative technique: Bragg conversion in crystal Experimental limits on solar axion flux from dark-matter experiments (SOLAX, COSME, DAMA, CDMS ...) Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Pointing a Magnet to the Sun
By CAST student Sebastian Baum Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Parameter Space for Axion-Like Particles (ALPs)
Two parameters: Weinberg Wilczek - ALP mass 푚 푎 “standard axion” - ALP-훾 coupling 푔푎훾
Model dependence (KSVZ, DFSZ, …) broadens 2 3 푔푎훾푚푎 the “axion line” Γ = 푎→훾훾 64휋
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Parameter Space for Axion-Like Particles (ALPs)
CAST exclusion range
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Parameter Space for Axion-Like Particles (ALPs)
CAST exclusion range End of solar spectrum
Large 푚푎, 푎-훾-oscillations suppressed
푎-훾-oscillations enhanced with He filling (푚훾 ∼ 푚푎)
Maximal mixing (“coherent”, small 푚푎)
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Parameter Space for Axion-Like Particles (ALPs)
- Improvement by a factor of 30
- Leaping into uncharted territory
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Parameter Space for Axion-Like Particles (ALPs)
- Improvement by a factor of 30
- Leaping into uncharted territory
Pushing generic ALP frontier
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Any Light Particle Search II (ALPS-II) at DESY
ALPS-I (finished)
ALPS-IIa (2014)
ALPS-IIb (2015)
ALPS-IIc (2017)
ALPS-II Technical Design Report, arXiv:1302.5647
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Shining TeV Gamma Rays through the Universe
Georg Raffelt, MPI Physics, MunichFigure from a talk by Manuel Meyer (Univ.Ultralight Hamburg) Frontier, MITP, Mainz 15–19 June 2015 Shining TeV Gamma Rays through the Universe
Georg Raffelt, MPI Physics, MunichFigure from a talk by Manuel Meyer (Univ.Ultralight Hamburg) Frontier, MITP, Mainz 15–19 June 2015 Parameter Space for Axion-Like Particles (ALPs)
ALPS-II at DESY
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Galactic Globular Clusters
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 New ALP Limit from Globular Clusters
Helium abundance and energy loss rate from modern number counts HB/RGB in 39 globular clusters
Planck Ayala, Dominguez, Giannotti, Mirizzi & Straniero, arXiv:1406.6053
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Axion and ALP Dark Matter
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Creation of Cosmological Axions by Re-alignment
푻 ~ 풇풂 (very early universe) 푉(푎)
• UPQ(1) spontaneously broken
• Higgs field settles in “Mexican hat”
• Axion field sits fixed at 푎𝑖 = Θ𝑖 푓푎 푎
푻 ~ ퟏ GeV (푯 ~ ퟏퟎ−ퟗ eV) 푉(푎) • Axion mass turns on quickly by thermal instanton gas
• Field starts oscillating when 푎 푚푎 ≳ 3퐻
• Classical field oscillations (axions at rest) Θ = 0
Axions are born as nonrelativistic, classical field oscillations Very small mass, yet cold dark matter
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Axion Cosmology in PLB 120 (1983)
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 WISPy Cold Dark Matter
General ALPs produced by re-alignment as cold dark matter
Arias, Cadamuro, Goodsell, Jaeckel, Redondo, Ringwald, arXiv:1201.5902
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Axion Dark Matter Driving Oscillators
4 Oscillating axion field (DM) ΛQCD Oscillating Q term • Drives oscillating neutron EDM Θ = 푎/f푎 • Drives oscillating E-field in microwave cavity w/ B-field −휋 +휋
3 Assume axions are the galactic dark matter: 휌푎 ~ 300 MeV/cm
2 2 2 2 2 2 2 4 휌푎 = 푚푎Φ푎 = 푚푎 Θ푓푎 ∼ Θ 푚휋푓휋 ∼ Θ ΛQCD
Independently of 푓 expect 푎 −19 Θ 푡 = 푎 푡 /푓푎 ∼ 3 × 10 cos 푚푎푡
16 Expect time-varying neutron EDM, MHz frequency for 푓푎 ~ 10 GeV
푒 푚푞 −34 푑푛∼ Θ ∼ 3 × 10 푒−cm cos 푚푎푡 2푚푛 푚푁
8 orders of magnitude below limit on static EDM, but oscillates! CASPEr Project
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Cold Axion Populations
Cosmic axion Scenario 1
Random string • Cosmic inflation first
Θ푖 values • PQ symmetry breaking at 푇 ∼ 푓푎 1.12 0.01 • Every causal patch has different random Θ푖 0.37 0.63 1.93 • Topological defects at interfaces
2.01 • Axion dark matter from 3.14 0.17 1.57 - average re-alignment - cosmic-string (CS) & domain-wall (DW) decay Scenario 2
• Cosmic inflation after PQ symmetry breaking
• All axions from re-alignment of one random Θ = 1.57 푖 Θi in our patch of the universe
• Allows large 푓푎 if Θ푖 ≪ 1 (“anthropic” case)
1.184 1.184 2 2 푓푎 2 10 휇eV 훺푎ℎ = 0.20 Θ푖 12 = 0.11 Θ푖 10 GeV 푚푎
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Isocurvature Constraints
B-modes in CMB would exclude
“anthropic” regime of large 푓푎
[GeV]
푎 푓
B-modes in CMB would suggest “large” 푚 Classic 푎
regime for dark matter axions Axion decay constant constant decay Axion
Hubble scale during inflation [GeV]
Visinelli & Gondolo, arXiv:1403.4594
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Axion Production by Domain Wall and String Decay Recent numerical studies of collapse of string-domain wall system
1.19 푓푎 Ω ℎ2 = 8.4 ± 3.0 푎 1012GeV
−0.41 푔∗,1 Λ × 70 400 MeV
Implies a CDM axion mass of
푚푎 ∼ 300 휇eV
Hiramatsu, Kawasaki, Saikawa & Sekiguchi, arXiv:1202.5851 (2012)
More recently by the same group
푚푎 ∼ 90 − 140 휇eV
Kawasaki, Saikawa & Sekiguchi, arXiv:1412.0789 (PRD 2015)
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Axion Dark Matter Density
Partly excluded by Hot DM Cold DM cosmic HDM bounds & Euclid sensitivity
[arXiv:1502.03325] JavierRedondo 2014
Realignment
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Axion Dark Matter from Topological Defects Editor’s suggestion
Diversity of scenarios for cosmic axion production depending on domain-wall index NDW and phase parameter δ of the bias term
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Pie Chart of Dark Universe
Dark Energy ~70% (Cosmological Constant)
Neutrinos ~ Ordinary Matter 5% 0.1-2% (of this only about Dark Matter 10% luminous) ~25%
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Historical Neutrino Dark Matter Lessons
Early 1980s - If neutrinos have mass, probably they are dark matter (풎흂~ퟏퟎ 퐞퐕) (“Neutrinos are known to exist”, only SM candidate)
- Detection of 풎흂풆 ∼ ퟑퟎ 퐞퐕 at ITEP, Moscow (PRL 58:2019, 1987) - Dedicated oscillation experiments (NOMAD 1995–1998 and CHORUS 1994–1997)
Status 2015 - 70% of gravitating “mass” is dark energy - Dark matter must be mostly “cold” (structure formation) - Neutrinos have sub-eV masses (oscillations, cosmo limits) - Sub-dominant dark matter component
History does not always repeat itself, but … - If axions (or similar) exist, MUST be ALL of dark matter?
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Dennis the Menace
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Landscape of Axion Searches
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 CP-Violating Forces
푁 푁 푁 푒 푒 푒 푔푠 푔푠 푔푠 푔푝 푔푝 푔푝
bulk bulk bulk spin spin spin 푎 푎 푎
Tests of Newton’s law Torsion balance using Spin-spin forces & equivalence principle: polarized electron spins hard to measure 푁 2 푁 푒 푒 2 Scalar axion coupling 푔푠 Axion couplings 푔푠 푔푝 Axion couplings 푔푠 T-violating force
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 NMR Experiment
ARIADNE: Axion Resonant InterAction DetectioN Experiment A.Geraci, A.Arvanitaki, A.Kapitulnik, Chen-Yu Liu, J.Long, Y.Semertzidis, M.Snow (to be supported by NSF and/or DoE?) Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 New Ideas for Axion Detection
IAXO
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP,[Arvanitaki Mainz 15–19 2015]June 2015 Axion and Axion-Like Particle Searches
ARIADNE WISP Center for Axion & Precision DMX Physics (KAIST, Korea) (DESY)
MAGIC ADMX-HF (Yale) Axion Dark Matter Experiment (UW, Seattle)
H.E.S.S.
IAXO Proposal CASPEr, perhaps @ HIM (CERN) (Mainz)
CAST @ CERN
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Dow Jones Index of Axion Physics
inSPIRE: Citation of Peccei-Quinn papers or title axion (and similar) 350
300
250
200
150
100
50
0
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015 Dow Jones Index of Axion Physics
inSPIRE: Citation of Peccei-Quinn papers or title axion (and similar) 350
300
250
200
150
100
50
0
Georg Raffelt, MPI Physics, Munich Ultralight Frontier, MITP, Mainz 15–19 June 2015