0 La Lac . - Breaks induces dn , orders limits of 10 - PowerPoint PPT Presentation

Axion phenomenology � � Recap of Strong CP problems and axions. Peccei-Quinn sectors � Couplings of axions to photons � Search for solar axions � Axions as possible dark matter candidates ��

Strong CP problem and axions � ¥0 La Lac → . - Breaks induces dn , orders limits of 10 above m ~ . da .+*EEIaj¢o if 5 OC ) meE1muE6⇒ - - . energy relax to \¥*gIYepIhF.acp vacuum → ° . Oeff Hag ° Quite = = . This of process relaxation not is instantaneous but happens a as , function of E DM �� be ⇒ can axcoug .

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Peccei-Quinn symmetry � exist ) models ( . model heavy of Consider very a generated by with quark mass Many#ht symmetry breaking spontaneous Lpa=Y(9←P +4214+4.2/42 +729 +YI49* ← Fatoyhmety °1→eit9 ;k→eit4< V(4)=X( 0*9 ? fay m¢=fa ⇒ + - Goldstone bosom 9 1 of the phase , . 4 Integrating zz9¥hGE out guy ��

Derivation of axion mass and coupling to EM � You anomaly got the to use z¥tmQqFE equation + 7(EffsE)=2mqEik9++fInGG @=aHa) QCD Lagrangian Take a + ¥541 - m)%ts9÷sGG Loa= tgcwcw - qieioeoa rotations apply and chiral r - Yz4←/mu)a - Yz(m*1md) E od 't = ; = mumd/( where ) Mutmd M* = . GE and This Efron removes it transfers quark to the sector �� .

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Stellar energy loss to axions � ⇐ '⇐t =E $ Primakoff Example process : Seen generates inside the 48=6×0 "s¥rw(,F¥a,§ 2481 got Must ( ) e- at Earth by fife Lr= Egy# - 4keV ��

- * Solar axions � § ⇐ : luminosity ,} Clearly , in axcosy } less should than of 1 -10% be luminosity solar d 1§y§ . \ problems ( 8 otherwise models ) ←x solar with . . . its ih \ detect Can we \ ? solar axioms \ interact ( remember , they very × Weekly ) ! ionization ! Look for extra * for Look regeneration in A j fields magnetic ��

Mixing of axions and photons in external B � sar ACEBJ ITFE → gay a . perpendicular field magnetic Create propagation to aandj ⇒ axiom will Propagation eigeumodes of mix . equation the satisfies = ( ←¥IBg¥ is (E) . m÷DtD Bgq × Ey=BsofIiw§=4Bm4ysnYgwm⇒ Pa→r(L)=sn%oeff)sm2( < maY4kr ) ��

CAST limits on g a γ� Notice additional exclusion from gas filling ) -1 (GeV ! a g -9 10 SUMICO 3 He 4 He HB stars -10 10 CAST Vacuum KSVZ [E/N = 0] Axion models HDM ALP axior - , , , Like -11 particles 's 10 -2 -2 -1 -1 10 10 10 10 1 1 m (eV) axion ���

Constraints on solar axions from Xenon 100 � Best direct constraints on g ae et - - get -9 10 Si(Li) DFSZ -10 10 XMASS Solar ! EDELWEISS Ae -11 10 g ¥dH XENON100 KSVZ -12 10 . Red giant -13 10 -5 -4 -3 -2 -1 10 10 10 10 10 1 2 m [keV/c ] A examples all Unfortunately these in , ~ g4g the signal scales as ��� .

IAXO? � Significant gain over CAST ��� $./0/12033------456$-,789- !!"!#$%&'#()(*+,-

“Hints” on ALPs and axions Alps - Like axiom particles . ( relation strict between me and f- is ) telexed [Horns 15] New hints on ALPs: anomalous transparency of the Universe to the TeV gamma rays; anomalous cooling of neutron star in Cas A(?); preference for extra energy loss channels by comparing HB and RGB stars in globular clusters etc. (After A Ringwald’s talk) ���

Cosmological evolution of a massive scalar � d1#a Mah � 1 � a = = - - ii 3H°a mia + + =o oscillator similarity with ( notice ) friction with ( szttcnpradjknthpl izlr It H= = = foe → Matainftiaf fimhah ' = p diluted \ i getting by c} \ Hubble expansion byR na H When < Me ���

Cosmological evolution of axion field � MACD that models Large 1- ' ( ,fT=aD3kCa⇒ 5×03 L2 - - for smaller s#Hd4d3ay ( 1=3464.2 2×104 Shati - window " Aaron , 109641 fa £ Astrophysics Cosmology - negotiable depends On non on ���

“Axion haloscopes” × 105¥ Ma dear - - -µeV mell ⇒ range . = fEsgqowf.oajhjooasi.ktespgitactie-o.3codycais-mkechtelflh-ttxloYn@u.tt ���

WIMP phenomenology � � WIMP abundance via the annihilation cross section � Example with the Higgs-mediated scalar dark matter � Scattering on nuclei. Perspectives of direct detection. � WIMPs with extra mediators. Secluded WIMPs DM D= -qq€ SNL < Mpm ���

Expansion-stopped self-annihilation � egecakou Boltzmann - ny R→d(nR34de=<ot>(n⇐a2 % When RHS e- Naa n to = at To - m . , when Annihilation stops rate Hubble tony okdnea < = = ' ftp.grftaten.us bgR ���

Expansion-stopped self-annihilation � if Shxtshmn 0.24 503bar tpbn ( ) Tamil = C × = weak to similar many - Very sections scale cross . Accident ? interacting weakly case for Of a particles ? hashve ���

Lee-Weinberg window on WIMPs � between Suppose that interactions SM and wimps are - type :* = forces weak gowFy9¥ by nelaxthisassunyg small GIM mediated > ← ,sm . = Mom % = 4 4 high GW - m ,5m ~ Man tpbn = fewcoey mam Min - - tasoftef mom 6611 hear ~ neutrinos exatee ���

Higgs-mediated dark matter example � models srmplest One the Wimp of ; =3 1155 L sjj⇒± - §,E# Higgs portal +7(H#s2 YzmIns2 a- breaking EW symmetry V=z46E÷ H+H=E(v7w0+$ H = 2252 terms HS2 ; interaction msIMo2ttv2 - - -14mHz It alpbn > " ���

� � � � Simplest models of Higgs mediation Silveira, Zee (1985); McDonald (1993); Burgess, MP, ter Veldhuis(2000) ! ! DM through the Higgs portal – minimal model of DM ! ! 4 S 4 + m 2 − L S = λ S 2 S 2 + λS 2 H † H 0 ! t = aapliy or >am ! ⇒ < - 00 = λ S 4 S 4 + 1 EW ) S 2 + λv EW S 2 h + λ ! 2( m 2 0 + λv 2 2 S 2 h 2 , 0 ! 2 – very small ! 125 GeV Higgs is “very fragile” because its with is ~ y b R = ! SM modes /( ! SM modes + ! DM modes ). Light DM can kill Higgs boson easily (missing Higgs ! : van der Bij et al., 1990s, Eboli, Zeppenfeld,2000) ! 10 -34 1 → SS !"#$$ � $%&'(#)*+&,**-*.)#",/0(1%2*'#*)3&0%#)4 10 -36 0.8 10 -38 7 0.6 10 -40 5 0.4 77 10 -42 777 0.2 ��� 10 -44 16 20 40 60 80 100 0.1 1 10 50 6789*8/$$.:%;4

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Nuclear recoil from interaction with WIMPs � Typical 1¥ particle A ~lo→c all loo . - it that . has energy - elastic nuclei with in share can Wimpgala=tg collision amplitude If the ' DM ' , hay , nuclear g- . a independent tr spm - there component B am , by enhancement number A the , - of mucboug inside nucleus ��� a

Nuclear recoil from interaction with WIMPs � %m # G=-mnY%D 92=-42 2¥ . 2 Eun = 847 405£ ,s)÷(mraD* man . >m^ 20.15×5139 GeV÷ 10-101 ~ I. , ,= a÷ 38 4×10 = ��� .

� � � � � Updates on the minimal Higgs-mediated model: 0 . 5 � 0 1 XENON100 (2012) = 5 0 . 0 Ω DM × / 0 Ω S 0 � 1 − 1 N − 0 . 5 log 10 λ hs log 10 λ hs O N Γ h → SS E 0 X 2 � × − 1 . 0 − 2 XENON100 (2012) 0 0 XENON100 × 5 1 N O XENON100 × 20 − 1 . 5 Ω S / Ω DM = 1 N � T E T 1 X 1 − 3 N N O O − 2 . 0 N N E E X � X 45 50 55 60 65 70 2 . 0 2 . 5 3 . 0 3 . 5 � m S (GeV) log 10 ( m S / GeV) Figure from Cline, Scott, Kainulainen, Weniger, 2013. � � Direct detection is competitive with the Higgs constraints. � � � New generation of direct detection can probe up to TeV scale WIMP masses. � � Higgs portal may lead to other forms of dark matter, e.g. based on the non-Abelian “dark group”, Hambye, 2008. ���

WIMP-nucleon scattering cross section � ¥ ± p ,n × ( gnn )2 G=mn2 O= 153 zoomed ~ ghn Foot ~ . &h mediated -6 - 10 ~ . mediated - - ���