Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://nuclphys.sinp.msu.ru/conf/lpp14/220809/Rashba.pdf Äàòà èçìåíåíèÿ: Wed Sep 16 16:31:17 2009 Äàòà èíäåêñèðîâàíèÿ: Tue Oct 2 00:40:08 2012 Êîäèðîâêà: Ïîèñêîâûå ñëîâà: m 106

Axions Astrophysical searches Summary

Search for axion-like par ticles in astrophysical obser vations
Timur Rashba
MPI (Katlenburg-Lindau, Germany) and IZMIRAN (Troitsk, Russia)

14th Lomonosov Conference, Moscow, August 19-25, 2009

Timur Rashba

Search for axion-like par ticles in astrophysical observations


Axions Astrophysical searches Summary

Outline

1

Axions Motivations Axion-photon interaction Astrophysical searches Shining light through the Sun Gamma-ray astronomy and axions Summary

2

3

Timur Rashba

Search for axion-like par ticles in astrophysical observations


Axions Astrophysical searches Summary

Motivations Axion-photon interaction

Outline

1

Axions Motivations Axion-photon interaction Astrophysical searches Shining light through the Sun Gamma-ray astronomy and axions Summary

2

3

Timur Rashba

Search for axion-like par ticles in astrophysical observations


Axions Astrophysical searches Summary

Motivations Axion-photon interaction

Motivations for axions
Strong CP problem and dark matter QCD Lagrangian: 1 L = - TrGµ G 4
µ

-

nf g 2 ~ TrGµ G 32 2

µ

¯ + i µ Dµ - Mq e

i

5



contains CP violating term: LCP = - g2 ~ TrGµ G 32 2
µ

Neutron electric dipole moment dn 10
-16

Problem: why so small? < 10-
9

e · cm < 10

-25

e · cm

Timur Rashba

Search for axion-like par ticles in astrophysical observations


Axions Astrophysical searches Summary

Motivations Axion-photon interaction

Strong CP problem: dynamical solution
Peccei&Quinn'77, Wiczeck'78, Weinberg'79

Postulate new global U(1) symmetry - Peccei-Quinn symmetry Re-interpret as a scalar field a - axion - Nambu-Goldstone boson LCP = - g2 ~ TrGµ G 32 2
µ

= LCP = -

g 2 a(x ) ~ TrGµ G 32 2 fa

µ

CP-symmetry dynamically restored
V(a)

Axion mass ma
a 0
Timur Rashba Search for axion-like par ticles in astrophysical observations

6.0 eV f m fa fa /106 GeV


Axions Astrophysical searches Summary

Motivations Axion-photon interaction

Outline

1

Axions Motivations Axion-photon interaction Astrophysical searches Shining light through the Sun Gamma-ray astronomy and axions Summary

2

3

Timur Rashba

Search for axion-like par ticles in astrophysical observations


Axions Astrophysical searches Summary

Motivations Axion-photon interaction

Axion-photon conversion/oscillations
Raffelt and Stodolsky, 1988

i z = - ( + ) ,

A = A , a m =
2 ma , 2



p 0 a B , 2M



0 p a

a a m

p =

2 p , 2

a =

- M = ga1

Photon-axion conversion probability P losc = M
2 a

= M

4B 2
2

2

-
2

2 p

22 ma

+ 4B ,

2

2

sin2

z los

,
c

4 M
2 2 p - ma

B = const ,

p = const

+ 4B 2

2

Timur Rashba

Search for axion-like par ticles in astrophysical observations


Axions Astrophysical searches Summary

Motivations Axion-photon interaction

"Shining light through the wall"
Solar axions CAST arXiv:0810.4482, Tokyo helioscope arXiv:0809.0596, . . . X-rays from the Sun with axion signatures
Zioutas et al, arXiv:0903.1807, Hannah et al, astro-ph/0702217; Davoudsial, Huber 2006, . . .

Detection of laser photons "through the wall"
ALPS, arXiv:0905.4159; GammeV, arXiv:0908.1529 [hep-ex], . . .

Detection of high energy photons from very distant astrophysical objects (gamma-ray telescopes, groundbased and satellite)
Simet, Hooper, Serpico, arXiv: 0712.2825; Angelis et al, arXiv:0807.4246; Fairbairn, TR, Troitsky arXiv:0901.4085; Bassan, Roncadelli arXiv:0905.3752; Burrage et al arXiv:0902.2320; Sanchez-Conde et al, arXiv:0905.3270; Hochmuth, Sigl arXiv:0708.1144 ...

Appearance of photons from nowhere (dark matter or cosmic axions search)
ADMX, astro-ph/0603108; Fairbairn et al arXiv:0706.0108; . . .

Timur Rashba

Search for axion-like par ticles in astrophysical observations


Axions Astrophysical searches Summary

Motivations Axion-photon interaction

CAST - CERN axion solar telescope
"Axion helioscope" technique Sikivi Strong magnet B = 9 Tesla, L = 9.26 m (LHC test magnet) x-ray detector at the end of pipe Observes the Sun 1.5 hour at both sunrise and sunset Expected axion flux: (ga /(10-10 GeV-1 ))2 3.75 â 1011 cm-2 s Average solar axion energy 4.2 keV Variable-pressure gas filling Primakoff effect
a e, Ze
virtual

e, 1983

-1

a B



virtual

Timur Rashba

Search for axion-like par ticles in astrophysical observations


Axions Astrophysical searches Summary

Motivations Axion-photon interaction

CAST and other limits
Zioutas, Tsagri, Papaevangelou, Dafni, arXiv:0903.1807

ga (GeV-1)

10-4 10-5 10-6 10
-7 RBF

Laser exps.

10-8 10-9 10-10 10
-11

Sumico
HB stars
HDM

CAST
Overclosure

10-12 10-13 10-14 10-15 10-16 -7 10

= 0]

Microwave cavity

[E/N KSVZ

models

Axion

10-6

10-5

10-4

10-3

10-2

10-1

1 10 maxion(eV)

Timur Rashba

Search for axion-like par ticles in astrophysical observations


Axions Astrophysical searches Summary

Motivations Axion-photon interaction

Cooling limits and dark matter
Globular cluster stars Cooling of red giants by + A A + a: ga < 10-10 GeV-1 Axions as a hot dark matter Thermal axions can form hot dark matter, but the axion decay into photons leads to limit: ma < 1 eV Hannestad, Mirrizi, Raffelt' Axions as a cold dark matter Axions can be a dominant cold dark matter component with mass ma > 10 µeV Hannestad, Mirrizi, R Can be probed by ADMX (microwave resonator in magnetic field) 1µeV< ma < 100µeV
affelt'05 Raffelt, hep-ph/0611118

05

Timur Rashba

Search for axion-like par ticles in astrophysical observations


Axions Astrophysical searches Summary

Motivations Axion-photon interaction

Axion Bounds
[GeV] f 10 m
3 a

10

6

10 eV

9

10

12

10

15

keV
a

meV

PeV
Direct ADMX searches CARRACK

neV

Experiments

Tele
scope

CAST

Too much hot dark matter Globular clusters (a- J- coupling) Too many events Too much energy loss

Too much cold dark matter (classic)
Classic region Anthropi c region

SN 1987A (a-N-coupling)

Georg Raffelt, Max-Pl anck-Instit ut fÝr Physik, MÝnchen, Germany

Timur Rashba

Search for axion-like par ticles in astrophysical observations

IPMU Coll oqui um, 10 June 2009, Tok yo, Japan


Axions Astrophysical searches Summary

Shining light through the Sun Gamma-ray astronomy and axions

Outline

1

Axions Motivations Axion-photon interaction Astrophysical searches Shining light through the Sun Gamma-ray astronomy and axions Summary

2

3

Timur Rashba

Search for axion-like par ticles in astrophysical observations


Axions Astrophysical searches Summary

Shining light through the Sun Gamma-ray astronomy and axions

Astronomy

Astronomers Studying an Eclipse by Antoine Caron (1571)
Timur Rashba Search for axion-like par ticles in astrophysical observations


Axions Astrophysical searches Summary

Shining light through the Sun Gamma-ray astronomy and axions

Solar occultation of 3C 279 -ray source?
271 sources in 3EG cataloge 101 identified 1 occulted by the Sun 3C 279 (brightest QSO) ecliptic latitude 0.2 once per year, October 8 occultation period 8.5 hours 3C 279
5 3C 273

Declination

0

-5

3C 279

-10 200

195 190 Right Ascension

185

Timur Rashba

Search for axion-like par ticles in astrophysical observations


Axions Astrophysical searches Summary

Shining light through the Sun Gamma-ray astronomy and axions

Shining light through the Sun by axions
Fairbairn, T.R., Troitsky, astro-ph/0610844

Probaility of photon emerging
1

Co n d i t i o n s
1 . 0 0 0 . 0 0 0 . 0 0 0 0 . 0 m g n g e e n o p o r P h ) ( t i

axion mass: ma 10-3 eV
1

inverse coupling: M= 105 - 106 GeV photon energy: around GeV
0 1 0 1 x 1 ) m c ( h t p e d 9 0 m 1 u x 1 m i x a m

V

V

V

e

e

e

G

G

G

n

5

5

6

o

t

0

0

0

1

1

1

o

h

x

x

x

1

1

3

p

1

1

Timur Rashba

Search for axion-like par ticles in astrophysical observations


Axions Astrophysical searches Summary

Shining light through the Sun Gamma-ray astronomy and axions

Solar halo and disk emission
Orlando, Strong, A&A, 480, 847 (2008)

Upper figure: Model angular profile of the solar emission above 100 MeV. Lower figure: Inverse-Compton emission modelled for a region of 10 from the Sun for 300-500 MeV. Intensity is given in cm-2 s-1 sr-1 .


Sum of disk and extended components of solar emission (10-7 cm-2 s-1 ). Energy solar Total (MeV) disk flux >1 0 0 0 .5 4 ±0 .3 2 4 .4 4 ± 2 .0 3
Fairbairn, T.R., Troitsky, arXiv:0809.4886
occult 3C 279 3C 279

F F

`+´ 6.2-3..7 · 10-7 cm-2 s-1 27 (8.6 ± 0.5) · 10-7 cm-2 s-
Timur Rashba

1

Search for axion-like par ticles in astrophysical observations


Axions Astrophysical searches Summary

Shining light through the Sun Gamma-ray astronomy and axions

Fermi Gamma Ray Space Telescope (GLAST)
number of photons
100

10
1 1 3 3 occultation survey mode occultation pointing mode occultations pointing mode occultations pointing mode 1-hour bin

Launched in June 2008 E = 30 MeV to 300 GeV Sensitivity about 50 times that of EGRET at 100 MeV Fermi goals:
par ticle acceleration in AGNs, pulsars, and SNRs resolve the -ray sky -ray bursts probe dark matter and early Universe
Timur Rashba
1 0 0.1 0.2

= 0.283 0.3

[degrees]

0.4

0.5

0.6

0.7

0.8

0.9

1

1.1 EGRET (rest of v.p. 11.0) 1 0.9 0.8 0.7 0.6 0.5 0.4 0.3 0.2 0.1 0 -1 -0.8 -0.6 -0.4 -0.2 0 0.2 0.4 = 0.283 0.6 0.8 1
EGRET (1991) Fermi (pointing mode)

Normalized flux

Time in degree units

Search for axion-like par ticles in astrophysical observations


Axions Astrophysical searches Summary

Shining light through the Sun Gamma-ray astronomy and axions

Outline

1

Axions Motivations Axion-photon interaction Astrophysical searches Shining light through the Sun Gamma-ray astronomy and axions Summary

2

3

Timur Rashba

Search for axion-like par ticles in astrophysical observations


Axions Astrophysical searches Summary

Shining light through the Sun Gamma-ray astronomy and axions

-ray astronomy
Predicted in 40s Detected in 60s -rays absrobed by atmosphere Ballons Satellites (recent INTEGRAL, EGRET, Fermi, ...) Atmospheric imaging Cherenkov telescopes (H.E.S.S., MAGIC, VERITAS, ...) Sources: AGN, pulsars, SNR, secondary cosmic rays
Timur Rashba Search for axion-like par ticles in astrophysical observations


Axions Astrophysical searches Summary

Shining light through the Sun Gamma-ray astronomy and axions

Photon attenuation length

Universe is not transparent for photons of energies above 1 TeV because of extragalactic background light (EBL)

3

protons

2

nearest BL Lac

(L/Mpc) log
10

1

0 photons -1 neutrons -2

-3 10

12

14

16

18
10

20

22

24

log

(E/eV)

Sanchez-Conde et al arXiv:0905.3270

Fairbairn, TR, Troitsky, arXiv:0901.4085

Timur Rashba

Search for axion-like par ticles in astrophysical observations


Axions Astrophysical searches Summary

Shining light through the Sun Gamma-ray astronomy and axions

3C 279 obser vation by MAGIC

Timur Rashba

Search for axion-like par ticles in astrophysical observations


Axions Astrophysical searches Summary

Shining light through the Sun Gamma-ray astronomy and axions

Axion-photon mixing in astrophysical objects
Fairbairn, TR, Troitsky, arXiv:0901.4085
M 1010 GeV axion 15 AXP NS GRB 10 GRB 5 5 15 PSR

5 0
Log10 B G

10

BLR MW NLR lobes jets clusters IG

Log B G

jets RG,BL 0 AD Sy K, HS, L clusters jets Sy 10

Log10 B G

BH Sy

BH RG,BL AD RG,BL

BLR 0 NLR lobes jets 5 MW clusters 10

5 10 15 20 6

5

starbursts voids

IG

15 15 10 5 Log R kpc 0 5

3

6

9 Log10

12 eV

15

18

3

0 3 Log10 ne cm

6
3

9

Photon-axion conversion probability P losc = M
2 a

= M

4B 2
2

2

-
2

2 p

22 ma

+ 4B ,

2

2

sin2

z los

,
c

4 M
2 2 p - ma

B = const ,

p = const

+ 4B 2

2

Timur Rashba

Search for axion-like par ticles in astrophysical observations


Axions Astrophysical searches Summary

Shining light through the Sun Gamma-ray astronomy and axions

Correlation of UHECR events with BL Lacs
Charged par ticles are deflected in IGMF and in GMF Neutral par ticles are absorbed at > 1018 eV, > 100Mpc Correlation of AGASA, Yakutsk, HiRes UHE events with BL Lacs, Tinyakov, Tkachev,
astro-ph/0102476; Gorbunov et al, astro-ph/0406654
180 30 60 60 30 60 30

Fairbairn, TR, Troitsky arXiv:0901.4085

180

Cannot be (shower development) Milky way galactic magnetic field model Harari, Mollerach, Roulet, astro-ph/9906309 HMR Probability of correlation is higher in the low panel (exposure + magnetic field) than upper (exposure) Correlation by chance is about 2.4% Axions parameters: mass 10-7 eV, coupling 10-10 GeV-1
Timur Rashba

180 30 60

180

Search for axion-like par ticles in astrophysical observations


Axions Astrophysical searches Summary

Shining light through the Sun Gamma-ray astronomy and axions

Other effects of axionlike par ticles in astrophysical obser vations
Detection of TeV photons from blazars
Simet, Hooper, Serpico, arXiv:0712.2825

White dwarf luminosity function
Isern, Garcia-Berro, Torres, Catalan, arXiv:0806.2807

Large-scale correlation in polarization of quazars
Payez, Cudell, Hutsemekers, arXiv:0805.3946

Polarization of extragalactic radio sources
Payez, Cudell, Hutsemekers, arXiv:0805.3946

Solar X-rays
Zioutas et al, arXiv:0903.1807

...

Timur Rashba

Search for axion-like par ticles in astrophysical observations


Axions Astrophysical searches Summary

Summar y
Axion-like par ticles (ALP) can be searched in astrophysical observations. In case of discovery they could provide significant contribution to dark matter, depending on their masses; Continuous effor t in exploring of axion-like par ticle parameters is taken in laboratory experiments using helioscopes (CAST, Tokyo), cavity experiments (ADMX and others) and laser experiments (ALPS and others); Many interesting effects with axion-like par ticles could be searched using atmospheric imaging Cherenkov telescopes (H.E.S.S., MAGIC and future CTA) and space-based telesopes (Fermi).

Timur Rashba

Search for axion-like par ticles in astrophysical observations