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

SLIDE 1

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

SLIDE 2

Strong CP problem and axions

La . → Lac

.+*EEIaj¢o

Breaks

¥0

, induces dn ~ 10

rders
f

m . above limits if 5

OC )

. da

meE1muE6⇒

to relax

\¥*gIYepIhF.acp

vacuum

energy

→ ° . Oeff = Quite

Hag

= ° . This process

f

relaxation is not instantaneous , but happens as a function

f

E ⇒ axcoug can be DM .

SLIDE 3

The need for UV completion.

La =

f

§Iy.Gj¢o

dm

perator

E. .immune . UV divergent diagram induces

(7af2^uqI

corrections . A UV completion B needed at energy scale £ fa . ⇒ Pecoei

Quinn

sectors

SLIDE 4

Peccei-Quinn symmetry

(

Many#ht

models exist ) . Consider a model

f

very heavy quark with mass generated by spontaneous

symmetry

breaking

Lpa=Y(9←P

+4214+4.2/42

+729

+YI49*

°1→eit9

;k→eit4<

← Fatoyhmety V(4)=X( 0*9

fay

? ⇒ m¢=fa + 1 Goldstone bosom , the phase

f

9 . Integrating

ut

4 guy zz9¥hGE

SLIDE 5

Derivation of axion mass and coupling to EM

You got to use the anomaly equation + z¥tmQqFE

7(EffsE)=2mqEik9++fInGG

Take a QCD Lagrangian @=aHa) Loa=

tgcwcw

+ ¥541

m)%ts9÷sGG

qieioeoa and apply chiral rotations r E =

Yz4←/mu)a

;

d

=

Yz(m*1md)

't where M* = mumd/( Mutmd ) . This removes Efron GE and transfers it to the quark sector .

SLIDE 6

Derivation of axion mass and coupling to EM

Up to 02 terms , you get L = 0° terms +

2m*fiirsu+dir¥0

← mass + Yzm

.IE#+nt.E)o2

toraaon ( Remember

.lt#tiTyo=afa)

tn QCD C In > =< Id > =

mI#.
(

Mutmd ) 02 term = axiom mass , Ma2= .m*2#YfaDmmj÷n , ( Ma =6meV x 109qe÷)

couphy

to pt : AFEWFI,ejIs4m±m 3( Mutmd ) You can derive this coupling from the same chiral rotation

SLIDE 7

Stellar energy loss to axions

⇐

'⇐t

=E

Example : Primakoff process $ inside the Seen generates

48=6×0 "s¥rw(,F¥a,§

got

2481 e- Must ( at Earth ) by

fife

Lr=

Egy#

4keV

SLIDE 8

Solar axions

§ Clearly, luminosity in axcosy

1§y§

should be less than

10%
f

1

}

solar

luminosity

. (

therwise

problems 8 \ d with solar models )

←x

:

*

. . .

⇐

,}

its \ ih Can we detect \ solar axioms ? \ ( remember , they interact very × Weekly ! ) * Look for extra ionization ! A Look for j regeneration in magnetic fields

SLIDE 9

Mixing of axions and photons in external B

ITFE

a gay → sar ACEBJ . Create magnetic field perpendicular to axiom propagation ⇒ aandj will mix . Propagation

f

eigeumodes satisfies the equation is (E) = (

←¥IBg¥

Bgq

× . m÷DtD

Pa→r(L)=sn%oeff)sm2(

< maY4kr)

Ey=BsofIiw§=4Bm4ysnYgwm⇒

SLIDE 10

CAST limits on gaγ

Notice additional exclusion from gas filling (eV) axion m

2

10

1

10 1 )

1

(GeV ! a g

11

10

10

10

9

10 SUMICO HB stars Axion models KSVZ [E/N = 0] HDM CAST Vacuum He 4 He 3

2

10

1

10 1 ALP

,

, axior , Like particles 's

SLIDE 11

Constraints on solar axions from Xenon 100

Best direct constraints on gae ] 2 [keV/c A m

5

10

4

10

3

10

2

10

1

10 1 Ae g

13

10

12

10

11

10

10

10

9

10 ! Solar Red giant Si(Li) XMASS EDELWEISS DFSZ KSVZ XENON100 et

get

¥dH

. Unfortunately , in all these examples the signal scales as ~ g4g .

SLIDE 12

IAXO?

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

SLIDE 13 “Hints” on ALPs and axions [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) Alps

axiom

Like particles . ( strict relation between me and f- is telexed )

SLIDE 14

Cosmological evolution of a massive scalar

1 a =

d1#a

=

Mah

ii + 3H°a + mia =o ( notice similarity with

scillator

with friction ) H= izlr = It =

( szttcnpradjknthpl

foe

'

p

fimhah = Matainftiaf \ i c} getting diluted

by

\

→

na byR Hubble expansion When H < Me

SLIDE 15

Cosmological evolution of axion field

Large 1- models that MACD

L2
5×03

(,fT=aD3kCa⇒

' smaller for Shati

2×104

( 1=3464.2

, Aaron window " 109641 £

fa

s#Hd4d3ay

Astrophysics Cosmology non

negotiable

depends

n

On

SLIDE 16

“Axion haloscopes”

Ma

dear

× 105¥

⇒

mell

µeV

range . = fEsgqowf.oajhjooasi.ktespgitactie-o.3codycais-mkechtelflh-ttxloYn@u.tt

SLIDE 17

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

qq€

SNL

D=

< Mpm

SLIDE 18

Expansion-stopped self-annihilation

Boltzmann egecakou

R→d(nR34de=<ot>(n⇐a2

ny

When RHS . to , n = Naa

e-

% at To m Annihilation stops when

tony

<

kdnea

= Hubble rate '

ftp.grftaten.us

=

bgR

SLIDE 19

Expansion-stopped self-annihilation

Shxtshmn

0.24 if ( Tamil ) = C × tpbn = 503bar Very similar to many weak

scale

cross sections . Accident ? Of a casefor

weakly

interacting hashve

particles ?

SLIDE 20

Lee-Weinberg window on WIMPs

Suppose that interactions between wimps and SM are

mediated

by

weak

type

forces

:*

gowFy9¥

=

nelaxthisassunyg . ← > =

GIM

,sm small = Mom % 4 4

high

~ GW m ,5m Man = tpbn

Min

mam

fewcoey

6611 hear mom ~

tasoftef

exatee neutrinos

SLIDE 21

Higgs-mediated dark matter example

One

f

the srmplest Wimp models ; L

=3

1155

YzmIns2

+7(H#s2

a- Higgs portal EW

symmetry

breaking H =

§,E#

V=z46E÷ HS2 ; 2252 interaction terms

msIMo2ttv2

sjj⇒±

14mHz

It

H+H=E(v7w0+$

" > alpbn

SLIDE 22

16

Simplest models of Higgs mediation Silveira, Zee (1985); McDonald (1993); Burgess, MP, ter Veldhuis(2000)! ! DM through the Higgs portal – minimal model of DM! ! ! ! ! ! 125 GeV Higgs is “very fragile” because its with is ~ yb 2 – very small ! 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)!

−LS = λS

4 S4 + m2 2 S2 + λS2H†H = λS 4 S4 + 1 2(m2 0 + λv2 EW )S2 + λvEW S2h + λ 2 S2h2, !"#$$$%&'(#)*+&,**-*.)#",/0(1%2*'#*)3&0%#)4 5 0.1 1 10 50 10-34 10-36 10-38 10-40 10-42 10-44 6789*8/$$.:%;4 7 77 777 20 40 60 80 100 0.2 0.4 0.6 0.8 1 <

r >am

⇒ t

aapliy

00

=

→ SS

SLIDE 23

Higgs-mediated dark matter example

.

k

1¥

tfmss colour 50 GeV , this process should dominate the Higgs width and dilute

bservable

modes . This does not happen ⇒ all masses below socoey are disfavored . LHC

ruby

ut

hzhtm

> Zoo

Higgs

mediated

Wimps

are

notated

SLIDE 24

Nuclear recoil from interaction with WIMPs

Typical

Wimpgala=tg

~lo→c . A loo all particle .

has
1¥

energy

that it can share with nuclei in elastic

collision

. , , ' ' DM If the amplitude g- hay a nuclear tr spm

independent

component , there B am enhancement

by

A , the number

f

mucboug inside a nucleus

SLIDE 25

Nuclear recoil from interaction with WIMPs

#

%m

2¥

92=-42

. 2

Eun

=

G=-mnY%D

847 . man >m^

405£

,s)÷(mraD*

~ 10-101

I. , ,=

20.15×5139 GeV÷ 38 = 4×10

a÷

.

SLIDE 26

Updates on the minimal Higgs-mediated model:
ΩS/ΩDM = 1

Γh→SS XENON100 (2012) XENON100 × 5 XENON100 × 20 X E N O N 1 T 45 50 55 60 65 70 mS (GeV) −3 −2 −1 log10 λhs ΩS / ΩDM = 1 XENON100 (2012) X E N O N 1 × 5 X E N O N 1 × 2 X E N O N 1 T 2.0 2.5 3.0 3.5 log10(mS/GeV) −2.0 −1.5 −1.0 −0.5 0.0 0.5 log10 λhs 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.

SLIDE 27

WIMP-nucleon scattering cross section

¥

±

p ,n O= G=mn2 × ( gnn )2 zoomed ~

153

. ghn ~ Foot &h

mediated
6

.

mediated

~ 10

SLIDE 28

Progress in direct detection of WIMPs

8B PandaX!I 2015 DarkSide!50 2015 XENON100 2012 LUX WS2013 PandaX!II 2016 LUX WS2014!16 mWIMP ( GeV/c2 ) WIMP!nucleon cross section ( zb ) 10 1 10 2 10 3 10 4 10 5 10 !2 10 !1 10 10 1 10 2 10 3 WIMP!nucleon cross section ( cm 2 ) 10 !47 10 !46 10 !45 10 !44 10 !43 10 !42 sec- scat- scat- get

f

get nu- masses be-

f
Fig. 8 Parameter space for elastic spin-independent dark matter-

Lux results , 2016 Tofaediated 6

CREs#oI5

#

higgs

mediated

6 Direct detection disfavours many H

mediated

models in ~ few eoo a mass

ayEY