Dark Matter
description
Transcript of Dark Matter
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Dark Matter
Axion Dark Matter
Georg G. Raffelt, Max-Planck-Institut für Physik, München
Physics Colloquium, University of Sydney, 3 March 2014
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Axions as Cold Dark Matter of the Universe
Dark Energy ~70% (Cosmological Constant)
Neutrinos 0.1-2%
Dark Matter~25%
Ordinary Matter ~5%(of this only about 10% luminous)
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Neutron
ProtonGravitation (Gravitons?)
Weak Interaction (W and Z Bosons)
Periodic System of Elementary Particles
Electromagnetic Interaction (Photon)
Strong Interaction (8 Gluons)
Down
Strange
Bottom
Electron
Muon
Tau
e-Neutrino
m-Neutrino
t-Neutrino nt
nm
nee
m
t
d
s
b
1st Family
2nd Family
3rd Family
Up
Charm
Top
u
c
t
Quarks Leptons
Charge -1/3
Down
Charge -1
Electron
Charge 0
e-Neutrino need
Charge +2/3
Up u
Higgs
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Supersymmetric Extension of Particle Physics In supersymmetric extensions of the particle-physics standard model,
every boson has a fermionic partner and vice versa
Sleptons (, , …)Squarks (, , …)
SpinSuperpartner
0
1/2GluinosWinoZinoPhotino ()
1/2
3/2
Higgsino
Gravitino
1/2 Leptons (e, ne, …)Quarks (u, d, …)
1 GluonsW
Z0
Photon (g)0
2
Higgs
Graviton
Spin Standard particle
• If R-Parity is conserved, the lightest SUSY-particle (LSP) is stable• Most plausible candidate for dark matter is the neutralino, similar to a massive Majorana neutrino
Neutralino = C1 Photino + C2 Zino + C3 Higgsino
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Laboratory Searches for WIMP Dark Matter
Energydeposition
Recoil energy(few keV) is measured by• Ionisation• Scintillation• Cryogenic
Galacticdark matterparticle(e.g. neutralino)
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
WIMP Searches (Underground Physics)
COUPPPICASSO
XENONLUX, ZEPLIN
WARP, ArDM
DEAP/CLEANDAMA/LIBRAKIMS, XMASS
DRIFTGERDA
CDMSEDELWEISS
CRESSTROSEBUD
HeatPhonons
Charge Light
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
WIMP Cross Section Limits 2014Klaus Eitel, 2014
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
High- and Low-Energy Frontiers in Particle Physics
1027eV
Planckmass
GUTscale
Electroweakscale
QCDscale
Cosmologicalconstant
10241021101810151012109106103110− 310− 6
WIMP dark matter(related to EW scale, perhaps SUSY)
Axion dark matter (related to Peccei-Quinn symmetry)
𝑓 𝑎𝑚𝜋 𝑓 𝜋 / 𝑓 𝑎 𝑚𝜋 , 𝑓 𝜋
Accelerator Frontier
CERN
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Axion Physics in a Nut Shell
CP conservation in QCD byPeccei-Quinn mechanism
For fa f≫ p axions are “invisible”and very light
Axions a ~ p0
mpfp mafa
g
ga
Particle-Physics Motivation
Axions thermally produced in stars, e.g. by Primakoff production
• Limits from avoiding excessive energy drain• Solar axion searches (CAST, Sumico)
ag
Solar and Stellar Axions
In spite of small mass, axions are born non-relativistically (non-thermal relics)
Cold dark matter candidate
ma ~ 10 meV (or much smaller or larger)
Cosmology Search for Axion Dark Matter
S
Nga
Bext
Microwave resonator (1 GHz = 4 meV)
Primakoffconversion
ADMX-LF (UW Seattle) ADMX-HF (Yale)
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
CP Violation in Particle Physics
Physics Nobel Prize 2008
Discrete symmetries in particle physicsC – Charge conjugation, transforms particles to antiparticles violated by weak interactionsP – Parity, changes left-handedness to right-handedness violated by weak interactionsT – Time reversal, changes direction of motion (forward to backward)CPT – exactly conserved in quantum field theoryCP – conserved by all gauge interactions violated by three-flavor quark mixing matrix
M. Kobayashi T. Maskawa
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
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
The CP Problem of Strong Interactions
ℒQCD=∑𝑞𝜓𝑞( i𝐷−𝑚𝑞𝑒
i 𝜃𝑞 )𝜓𝑞−14𝐺𝜇𝜈𝑎𝐺𝑎
𝜇𝜈−Θ𝛼 s
8𝜋 𝐺𝜇𝜈 𝑎~𝐺𝑎
𝜇𝜈
𝜓𝑞→𝑒❑−𝑖𝛾 5𝜃𝑞 /2𝜓𝑞
ℒQCD=∑𝑞𝜓𝑞 (i𝐷−𝑚𝑞)𝜓𝑞−
14𝐺𝐺− (Θ− arg det 𝑀𝑞)⏟
−𝜋 ≤Θ≤+𝜋
𝛼s8𝜋 𝐺~𝐺
Real quarkmass
Phase fromYukawa coupling
Anglevariable
CP-oddquantity
Remove phase of mass term by chiral transformation of quark fields
can be traded between quark phases and term No physical impact if at least one Induces a large neutron electric dipole moment (a T-violating quantity)
Experimental limits: Why so small?
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Neutron Electric Dipole Moment
Violates time reversal (T) andspace reflection (P) symmetries
Natural scale𝑒
2𝑚𝑁=1.06×10−14𝑒cm
Experimental limit|𝑑|=0.63×10− 25𝑒 cm
Limit on coefficient
Θ𝑚𝑞
𝑚𝑁≲10−11
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Strong CP Problem
+𝜋−𝜋 Θ
ΛQCD4
QCD vacuum energy
• CP conserving vacuum has (Vafa and Witten 1984)• QCD could have any , is “constant of nature”• Energy can not be minimized: not dynamical
Equivalent Equivalent
−2𝜋 +2𝜋
Peccei-Quinn solution: Make dynamical, let system relax to lowest energy
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
The Pool Table Analogy (Pierre Sikivie 1996)
GravitySymmetricrelativeto gravity
Pool table
New degree of freedom Axion
𝚯
(Weinberg 1978, Wilczek 1978)
Axis
Symmetrydynamicallyrestored
(Peccei & Quinn 1977)
Symmetrybroken
Floor inclined
fa
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
35 Years of Axions
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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)
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Axion Bounds and Searches
103 106 109 1012 [GeV] fa
eVkeV meV meVmaneV
1015
Directsearches
Too much CDM (misalignment)
TelescopeExperiments
Globular clusters(a-g-coupling)
SN 1987AToo many events
Too muchenergy loss
Too muchhot dark matter
CAST ADMX(Seattle & Yale)
Globular clusters (He ignition), WD cooling(a-e coupling)
Too much cold dark matter(re-alignment with Qi = 1)
Classicregion
Anthropicregion
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Dark Energy ~70% (Cosmological Constant)
Neutrinos 0.1-2%
Dark Matter~25%
Ordinary Matter ~5%(of this only about 10% luminous)
Axions as Cold Dark Matter of the Universe
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Creation of Cosmological Axions (very early universe)
• UPQ(1) spontaneously broken• Higgs field settles in “Mexican hat”• Axion field sits fixed at
𝑎
𝑉 (𝑎)
𝑎
𝑉 (𝑎)
Θ=0
( eV)• Axion mass turns on quickly by thermal instanton gas• Field starts oscillating when • Classical field oscillations (axions at rest)
Axions are born as nonrelativistic, classical field oscillationsVery small mass, yet cold dark matter
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Axion Cosmology in PLB 120 (1983)
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Killing Two Birds With One Stone
Peccei-Quinn mechanism• Solves strong CP problem• Provides dark matter in the form of axions
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Cosmic Axion DensityModern values for QCD parameters and temperature-dependent axion massimply (Bae, Huh & Kim, arXiv:0806.0497)
If axions provide the cold dark matter:
• implies GeV and meV (“classic window”)
• GeV (GUT scale) or larger (string inspired) requires (“anthropic window”)
Ω𝑎h2=0.195Θi
2( 𝑓 𝑎1012 GeV )
1.184
=0.105Θi2( 10𝜇eV
𝑚𝑎 )1.184
Θi=0.75( 1012 GeV𝑓 𝑎 )
0.592
=1.0 ( 𝑚𝑎
10𝜇eV )0.592
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Axion Production by Domain Wall and String DecayRecent numerical studies of collapseof string-domain wall system
Implies a CDM axion mass of
Hiramatsu, Kawasaki, Saikawa &Sekiguchi, arXiv:1202.5851 (2012)
Remains to be confirmed,interpretation of numerical studiesnot entirely straightforward
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
BEC Formation
• Axions ~ WIMP dark matter on scales axion Compton wavelength?• Larger-range correlation established by BEC dynamics? (Observable?)• Axions born as classical field oscillations → Issue of classical field dynamics (not a quantum effect)• BEC formation caused by gravitational interactions possible ???See also • Erken, Sikivie, Tam & Yang, arXiv:1111.1157 • Saikawa & Yamaguchi, arXiv:1210.7080 • Noumi, Saikawa, Sato & Yamaguchi, arXiv:1310.0167 • Davidson & Elmer, arXiv:1307.8024 • Berges & Jaeckel, arXiv:1402.4776
~100 citati
ons
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
High- and Low-Energy Frontiers in Particle Physics
1027eV
Planckmass
GUTscale
Electroweakscale
QCDscale
Cosmologicalconstant
10241021101810151012109106103110− 310− 6
WIMP dark matter(related to EW scale, perhaps SUSY)
Axion dark matter (related to Peccei-Quinn symmetry)
𝑓 𝑎𝑚𝜋 𝑓 𝜋 / 𝑓 𝑎 𝑚𝜋 , 𝑓 𝜋
Accelerator Frontier
CERN
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Searching for Solar Axions
Searching forAxion-Like Particles
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Experimental Tests of Invisible Axions
Primakoff effect:
Axion-photon transition in externalstatic E or B field(Originally discussed for by Henri Primakoff 1951)
Pierre Sikivie:
Macroscopic B-field can provide alarge coherent transition rate overa big volume (low-mass axions)• Axion helioscope: Look at the Sun through a dipole magnet• Axion haloscope: Look for dark-matter axions with A microwave resonant cavity
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Search for Solar Axions
g a
Sun
Primakoff production
Axion Helioscope(Sikivie 1983)
gMagnet S
Na
Axion-Photon-Oscillation
Tokyo Axion Helioscope (“Sumico”) (Results since 1998, up again 2008) CERN Axion Solar Telescope (CAST) (Data since 2003)
Axion flux
Alternative technique: Bragg conversion in crystal Experimental limits on solar axion flux from dark-matter experiments (SOLAX, COSME, DAMA, CDMS ...)
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Tokyo Axion Helioscope (“Sumico”)
Moriyama, Minowa, Namba, Inoue, Takasu & YamamotoPLB 434 (1998) 147Inoue, Akimoto, Ohta, Mizumoto, Yamamoto & MinowaPLB 668 (2008) 93
m
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
CAST at CERN
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Recent “shining-light-through-a-wall” or vacuum birefringence experiments:• ALPS • BMV • BFRT• GammeV • LIPPS • OSQAR • PVLAS
Photon Regeneration ExperimentsEhret et al. (ALPS Collaboration), arXiv:1004.1313
(DESY, using HERA dipole magnet) (Laboratoire National des Champs Magnétiques Intens, Toulouse) (Brookhaven, 1993) (Fermilab) (Jefferson Lab) (CERN, using LHC dipole magnets) (INFN Trieste)
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Shining TeV Gamma Rays through the Universe
Figure from a talk by Manuel Meyer (Univ. Hamburg)
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Parameter Space for Axion-Like Particles
𝜋η
𝑎WW
Invisibleaxion (DM)
Axion Line 𝝉𝒂→
𝟐𝜸 =𝝉U
𝜋η
𝑎WW
Invisibleaxion (DM)
Axion Line 𝝉𝒂→
𝟐𝜸 =𝝉U
HBStars 𝜋η
𝑎WW
Invisibleaxion (DM)
Axion Line 𝝉𝒂→
𝟐𝜸 =𝝉U
HBStars
CASTSolar Axions 𝜋η
𝑎WW
Invisibleaxion (DM)
Axion Line 𝝉𝒂→
𝟐𝜸 =𝝉U
HBStars
LaserExperiments
CASTSolar Axions
TeV g rays
How
to m
ake
prog
ress
?
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Next Generation Axion Helioscope (IAXO) at CERN
• Irastorza et al.: Towards a new generation axion helioscope, arXiv:1103.5334• Armengaud et al.: Conceptual Design of the International Axion Observatory (IAXO), arXiv:1401.3233
Need new magnet w/– Much bigger aperture: per bore– Lighter (no iron yoke)– Bores at Troom
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Searching for Axion Dark Matter
Searching forAxion Dark Matter
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Search for Galactic Axions (Cold Dark Matter)
Power
Frequency ma
Axion Signal
Thermal noise of cavity & detector
Power of galactic axion signal
Microwave Energies (1 GHz 4 meV)
Dark matter axions Velocities in galaxy Energies therefore
ma = 1-100 meV
va 10-3 c
Ea (1 10-6) maAxion Haloscope (Sikivie 1983)
Bext 8 Tesla
Microwave ResonatorQ 105
Primakoff Conversionga
Bext
Cavityovercomesmomentummismatch
4×10−21 W 𝑉0.22 m3 ( 𝐵
8.5 T )2 𝑄105×( 𝑚a
2𝜋 GHz )( 𝜌𝑎
5×10−25 g / cm 3 )
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Axion Dark Matter Experiment (ADMX), Seattle
Adapted from Gianpaolo Carosi
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
SQUID Microwave Amplifiers in ADMX
Adapted from Gianpaolo Carosi
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Axion Dark Matter Searches
1. Rochester-Brookhaven- Fermilab, PRD 40 (1989) 3153
2. University of Florida PRD 42 (1990) 1297
3. US Axion Search ApJL 571 (2002) L27
4. CARRACK I (Kyoto) hep-ph/0101200
123
4
Limits assuming axions are the galactic dark matter with standard halo
KSVZ
DFSZ
ADMX-LF (Seattle) search range (2015+)
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
ADMX-HF at Yale (Steve Lamoreaux Group)
Design of cavity & magnet
Dilution refrigerator above & below deck
ADMX-HF will also be a test-bed for innovative concepts,e.g. thin-film superconducting cavities
Adapted from Karl van Bibber
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
WISPDMX at DESY and MPIfR
208 MHz microwave cavities H1 detector
Microwave cavities: HERA – 50, 208, 500 MHz208 MHz cavity: resonant modes at 199, 295, 433, 524, 579, 707, 765, 832 MHzMagnets: DESY H1 1.1 T (solenoid), HERA 5 T (dipole), Receiver technology: MPIfR, Tn ~ 100 KPhase 1,2 – searches using available facilitiesPhase 3 – advanced searches with specially designed facilities
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Broadband Approaches„Focusing“ the DM signal w/ spherical reflector
Feasible above 10 GHzTOKAMAKs:- Optimize B2V factor in a radiometer mode- Good at low frequencies- Design study under way (Lobanov et al. 2013)
TOKAMAKFacility
B[T]
V[m3]
B2V[T2 m3]
ToreSupra 4 30 480JET 4 200 3200ITER 5 1200 30000MPP ASDEX 3.1 14 135TEXTOR 3.0 7 63
Microwave cavity experiment
B[T]
V[m3]
B2V[T2 m3]
ADMX 7.6 0.2 11.5
WISPDMX 1.1 0.46 0.6
Horns et al. 2013
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Center for Axion and Precision Physics (CAPP)
New Institute for Basic Science (IBS), KoreaThe plan is to launch a competitive Axion Dark Matter Experiment in Korea, participate in state-of-the-art axion experiments around the world, play a leading role in the proposed proton electric-dipole-moment (EDM) experiment and take a significant role in storage-ring precision physics involving EDM and muon g–2 experiments.
15 Oct 2013
YannisSemertzidis
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
What if the axion is found?
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
1D Infall and the Folding of Phase Space
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Fine Structure in the Axion Spectrum• Axion distribution on a 3-dim sheet in 6-dim phase space• Is “folded up” by galaxy formation• Velocity distribution shows narrow peaks that can be resolved• More detectable information than local dark matter density
P.Sikivie& collaborators
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Axion Bounds and Searches
103 106 109 1012 [GeV] fa
eVkeV meV meVmaneV
1015
Directsearches
Too much CDM (misalignment)
TelescopeExperiments
Globular clusters(a-g-coupling)
SN 1987AToo many events
Too muchenergy loss
Too muchhot dark matter
CAST ADMX(Seattle & Yale)
Globular clusters (He ignition), WD cooling(a-e coupling)
Too much cold dark matter(re-alignment with Qi = 1)
Classicregion
Anthropicregion
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Oscillating Neutron EDM by Axion Dark Matter
Assume axions are galactic dark matter: 300 MeV/cm3
Independently of expect Expect time-varying neutron EDM, MHz frequency for GeV
8 orders of magnitude below limit on static EDM, but oscillates!
+𝜋−𝜋
ΛQCD4
Θ=a / f a Oscillating axion field (DM)→ Oscillating Q term→ Oscillating neutron EDM
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Searching for Axions in the Anthropic Window
Graham & Rajendran, arXiv:1101.2691Budker, Graham, Ledbetter, Rajendran & Sushkov, arXiv:1306.6089
CASPEr experimentPrecise magnetometry to measuretiny deviations from Larmor frequency
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Cosmic Axion Spin Precession Experiment (CASPEr)
Budker, Graham, Ledbetter, Rajendran & Sushkov, arXiv:1306.6089
Time-varying nucleon EDM caused by axion DM in Lead Titanate magnetometer
Phase I
Phase II
Magnetometer noise limit
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Helmholtz Institute Mainz (HIM)
Building under construction
New institute onStructure, symmetry and stability of matter and antimatter
Dmitry BudkerMoving from Berkeley to HIM
Plans to pursue CASPEr
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Dow Jones Index of Axion Physics
19771979
19811983
19851987
19891991
19931995
19971999
20012003
20052007
20092011
20130
50
100
150
200
250inSPIRE: Citation of Peccei-Quinn papers or title axion (and similar)
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Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Pie Chart of Dark Universe
Dark Energy ~70% (Cosmological Constant)
Neutrinos 0.1-2%
Dark Matter~25%
Ordinary Matter ~5%(of this only about 10% luminous)