Solar and other anomalies as imprints of new physics

K. Zioutas

University of Patras & CERN

My Collaborators since ~2000: V.Anastassopoulos (U.Patras), L. Di Lella (CERN)Th.Papaevangelou (Saclay), Y. Semertzidis (BNL)M.Tsagri (U.Patras)

++ librarians @ @ CERN & U. Patras Open Access! Open Access!

CERN Particle Physics Seminar18th September 2007

Konstantin.Zioutas@cern.ch

E. Arik, M. Asplund, Ch. Beck, H. Dahle, K. Dennerl, M.K. Georgoulis, M. Grande, Th. Hackman, S.H. Hansen, D.H.H. Hoffmann, J. Huovelin, J. Jacoby, B. Lakic, A. Liolios, A. Nordt, S. Orlando, A. Ortiz, K. Pedersen, S. Riemer-Sørensen, S. Solanki, Sp. Tzamarias, O. Vilhu, . . . .

CAST motivated work! sun↛ black box

ILIAS / EU

Profit / encouraged from :

OutlineOutline

• Indirect direct signatures• axions• Solar problems • Analysis of solar observations results

• Observations in X/γ-rays, CMBGC, CGs, VHE sources

The others?

solar physicists == skeptical, but..

generous use of (recent) citations

3

RHESSI light + massive ~axionsHINODE , YOHKOH

SMART

DRIFTGe, NaI underground exp’s

CAST

Missions / DM – exp’s searching for axions

axion-like

4

Quiet-Sun X-ray observationsRHESSI

Topic Feasibility Importance (1-10)

Microflares 10 1 (program calibration)Corona itself 1 3 (nonthermal tail?)CRAND halo 1 3 (physics is important)Diffuse background 1 2 (known source)Axions 1 10 (fundamental physics)General 10 2 ( get limits)

Hannah, I.G., Hurford, G.J, Hudson H.S, Lin, R.P, RHESSI: http://solar.physics.montana.edu/rhessi/projects/full_abstract.pl?entry=335

RHESSI

5

RHESSI Science nuggets, http://sprg.ssl.berkeley.edu/~tohban/nuggets/?page=article&article_id=16

AxionsAxions. .

Some could be trapped at the Sun, and these could decay into detectable X-rays, and RHESSI could detect them –it is a long shot, but well worth the observational effort..

RHESSI/NASA Exploring the Quiet Sun 2005, Hannah

6

List of observations incompleteList of observations incomplete (not) on purpose

So far: Constrains from stellar evolution / cooling escaping heat?

the bulk of the star evolutionlocal signatures more significant? this talk

(Un)solved central solar problems:

Light source? solar nuclear reactions

ν-deficit ~30 years ν-mass

Corona heating? 1937-

EUV/X- ray source? ~axi⊙⊙ns this work

7

Indirect astrophysical DM-signatures

WIMPs widely discussed axions? little “ this work (biased )

also: Bullet cluster ++ Abell 520 ≈ direct

8

Clowe, Bradac, Gonzalez, Markevitch, Randall, Jones, ZaritskyApJ. 648 (Sept. 2006) L109

The bullet cluster

“first direct proof for dark matter” 20062006

9

Abell 520

X-rays

lensing

Mahdavi , Hoekstra, Babul, Balam, Capak, ApJ.(Oct.2007) 10

Abell 520

X-rays

lensing

Searching for decaying axion-like DM from GCs

Riemer-Sørensen, Z., Hansen, Pedersen, Dahle, Liolios, PRL (2007).

11

innerSUN == source + target of neutrinos axionsaxions

mCP’s

(WIMPs)

…?++ its many mysteries @@ present

12

The Primakoff Effect 19511951H Primakoff

Behind all present axion work!

axionaxion

inside B?

13

γ

BXγvirtual

α

CASTCAST

P.P. Sikivie 1983Sikivie 1983

ubiquitous @ Sun

┌► X-rays, visible, …Unexpected (dis)appearance of photons in B

Lx ~ (gLB)2~ ρ mγ ≈ maxion coherence ≈ ∞

dynamical behaviourtransient effects

1. axion ⇄ photon oscillation!

2. axion→ 2γ decay of gravitationally trappedmassive ~axions, e.g. KK-type generic

▼ghost “plasma”

▼Lx ≈ constant

solar observations require both components15

• 11 years cycleOpen solar questions

16

Ramesh,SundararamanSolar Phys. 234(2006)393

EUVEUV

1992

BB

2000

X X ––r a y s

r a y s

Woods, Lean, Eparvier, ILWS workshop, GOA, Febr.19-24, 2006http://cdaw.gsfc.nasa.gov/publications/ilws_goa2006/145_Woods.pdf

Sunspot numbers

Solar activity

EUVEUV= = RoIRoI!!this work.

17

Yohkoh

Th. Papaevangelou

18

Lx vs. B

Lx ~ Bn =ƒ(time) YOHKOH / XRT

The relation between the solar soft X-ray flux (below ~4.4keV) …and B can be approximated by a power law ≈ 2.

characteristic for axion – photon conversion

Benevolenskaya, Kosovichev, Lemen, Scherrer, Slater ApJ. 571 (2002) L181Hoffmann, Z., Nucl. Phys. B S151 (2006) 35919

• 11 years cycle• Solar corona heating problem

Open solar questions

20

The enigma of coronal heatingone of the outstanding puzzles of stellar astronomy ++one of the most challenging problems in astrophysics.

Aschwanden, Adv. Space Res. 39 (2007) 1867Jefferies, McIntosh, Armstrong, Bogdan, Cacciani, Fleck, ApJL. 648 (2006) 151

Priest, Longcope, Heyvaerts, ApJ. 624 (2005) 1057

Inverted Temperature:

the coronal heating problem / paradox

Grotrian (1939)Solar Interior

108

107

106

105

104

103

Solar Corona

0 1

T[K]

RR⊙

21

Stellar observations ++ theory on stellar evolution:

↛↛ stars might possess atmospheres … that produce X-rays.Acton, Magnetodynamic Phenomena in the Solar Atm. (1996) 3

K Galsgaard, CE Parnell, A.& A. 439 (2005) 335RB Dahlburg, JA Klimchuk, SK Antiochos, ApJ. 622 (2005)1191

S Regnier, RC Canfield, Proc. SOHO 15 Workshop - Coronal Heating, St. Andrews, Scotland, 6-9 September 2004, ESA SP-575 (2004) 255

The magnetic field plays a crucial role in heating the corona …the exact energy storage & release mechanism(s) is(are) stillunknown . . . .the process by which it is converted into heat and other forms remains a nagging unsolved problem.

M.J. Aschwanden, A.I. Poland, D.M. Rabin, A.R.A.A. 39 (2001) 75C.J. Schrijver, A.A. van Ballegooijen, ApJ. 630 (2005) 552

Everything above the photosphere …would not be there at all.

~ ~ axionsaxions ……

2nd component

22

UV

5770K

http://www-sosst.larc.nasa.gov/meetings/2004/0615/presentations/08-kinnison.pdf

120eV 12 eV 3 eV

? Solar Spectral Irradiance

J.Lean,T.Woods11 years Irradiance Change: (Max-Min)/Min

λλ [nm]

λλ [nm]

?

23

Solar Atmosphere Earth Atmosphere

solar Xsolar X--ray selfray self--irradiation irradiation L. DiLella, K. Z. , Astropart. Phys. 19 (2003) 145gravitationally trapped KK-axions 22γγ

genericgeneric

Reconstructed X-ray spectrum non-flaring Sun @ solar minimum [X]

5050--100 MK100 MK??

[X] Peres, Orlando, Reale, Rosner, Hudson, ApJ. 528 (2000) 537

Tflare < 20MK

24

Reconstructed X-ray spectrum non-flaring Sun @ solar minimum

DiLella, Z., Astropart. Phys. 19 (2003) 145

KKKK--axionaxion modelmodel

generic

gaγγ≈10-13GeV-1

mKK≈10-3 eV

5050--100 MK100 MK??

??

25

inner / outer Sun

Reconstructed X-ray spectrum non-flaring Sun @ solar minimum

??1.8 MK

5050--100 MK100 MK??

B-modified solar axion spectrum??

innerSUN ~2MK @ 0.7Rsolar tachocline

the source? ? …how?

26

solar core

A. Mirizzi, 3rd Axion-WIMPs Workshop, Patras, June2007

B

LES ~axions

G. Raffelt

~5% Ltot-axionm=10eV & 100 Tesla

27

Z., Dennerl, DiLella, Hoffmann, Jacoby, Papaevangelou, ApJ. 607 (2004) 575

OFFPOINTINGS:OFFPOINTINGS:

1992 YOHKOH 2005- RHESSI

>43 days14.2.2007 14.2.2007 ––

2006- HINODEHINODE??

• Diffuse emission• Hydrostatic equilibrium↛↛ observations

2626thth Aug.:Aug.: JL Culhane,Adv Sp Res 19(1997)1839

Quiet Sun surface soft X-ray brightness

Radial distance

gaγγ

• 11 years cycle• Solar corona heating problem• B⊙

Open solar questions

29

BBsunsun ignored in ALL models

New axion source + axion conversion @@ Sun?

Yes, Yes, if ρplasma ∝ maxion ….

LES ~axions ‘near’ the surface

30

Chen, Hu, Sun, astro-ph/0705.3885, ApJ. 666 (Sept. 2007)

Chen, Hu, Xia, astro-ph/0705.3886, Adv. Space Res. (2007)

magnetic energy == main source for solar activity.B … poorly understood … … mysteries remain.

A. Reiners, G. Basri ApJ. 656 (2007) 1121

open question:open question:how magnetic energy how magnetic energy …… rapidlyrapidly …… creates solar explosions(?)such as flares ++ CMEs + catastrophic events.

Reiners, Basri ApJ. 656 (2007) 1121

http://solarscience.msfc.nasa.gov/maghstry.shtml

31

Livingston, Harvey, Malanushenko, Webster, Sol. Phys. 239 (2006) 41

Magnetic field in sunspotsMagnetic field in sunspots

measuredmeasured!!

locally?

5kGauss

32

Solar seismic models + the ν-predictions

103-104 T

30-100T

2-3 T

the internal rotation profileis not included in the study

new surprises may appear

Solar magnetic fields simulated. .

?(Primakoff)B » (Primakoff)E ? →→ Solar X-rays??Couvidat, Turck-Chieze, Kosovichev. ApJ. 599 (2003) 1434

> 105 T change solar ν-fluxes

33

11 Spruit, Scharmer, A&A 447 (2006) 343

• 11 years cycle• Solar corona heating problem• B⊙• Sunspots heat flux problem11

Open solar questions

34

The roots of the “tree”are still a mysterya mystery.

http://science.nasa.gov/headlines/y2001/ast07nov_1.htm

Below 4800 km … the roots of the sunspots are hotter than their surroundings, just the opposite of the surface

35

The origin of sunspots is not understood.The origin of sunspots is not understood.

Junwei Zhao, Dissertation, 2004, p.58http://soi.stanford.edu/papers/dissertations/junwei/thesis/PDF/thttp://soi.stanford.edu/papers/dissertations/junwei/thesis/PDF/thesis_double_page.pdfhesis_double_page.pdf

Energy budget OR heat flux problem @ sunspot

the sunspot Temperature (~4500K) is much higher as one would expect from complete suppression of convective energy transport.

http://gregor.kis.uni-freiburg.de/scientific.htmlSpruit, Scharmer, A.&A. 447 (2006) 343

36

Sola

r C

oron

a Pr

oble

mYOHKOH

heat flux problem @ umbra / penumbra

quiet Sunquiet Sun

Umbra

Temperature distributions

Nindos, et al., ApJ. SUPPL. 130 (2000) 485

Penumbra

Origin of Sunspots one of the great puzzles of astrophysicsZhao, et al., ApJ. 557 (2001) 384

PhotospherePhotosphere T ⇩⇩~4500K

Corona Corona T ⇧⇧B ~2 kG above most sunspots!

Spruit, Scharmer, A.&A. 447 (2006) 343

Some ARs are more productiveproductivity ⊗ B-configuration, as in the case of large flares.

Qiu et al., ApJ. 612 (2004) 530

37

SUNSPOTS originorigin??

Z., Dennerl, Grande, Hoffmann, Huovelin, Lakic, Orlando, Ortiz, Papaevangelou, Semertzidis, Tzamarias, Vilhu TAUP2005, J. Phys. Conf. Ser. 39 (2006) 103

(1=Q

uiet

Sun

)

50% of the quiet Sun

Solanki A&A Rev. 11 (2003) 153Plot reconstructed from:

• fundamental questions remain unanswered.• is an additional mechanism needed??

polarization?C. Beck

38

/ cm2 vs. July-Nov. 1996

van Driel-Gesztelyi, Démoulin, Mandrini, Harra, Klimchuk, ApJ.586 (2003) 579Z., Dennerl, Grande, Hoffmann, Huovelin, Lakic, Orlando, Ortiz, Papaevangelou, Semertzidis, Tzamarias, Vilhu, TAUP2005, J. Phys. Conf. Ser. 39 (2006) 103

The long-term evolution of AR7978

Yohkoh SXT

Lx∝ B1.94±.12

Eγ < 4 keV

Lx⇑

B [Gauss]

RHESSI :often hard X-rayemission from non-flaring ARs.

≳ 5 keVHannah, Hurford,Hudson, Abstract: 2005AGUFMSH11A0242HAGU Fall meeting, 5-9/12/2005

39

• 11 years cycle• Solar corona heating problem• B⊙• Sunspots heat flux problem11• Flares instantaneous particle acceleration

Open solar questions

40

Barnes, Leka, ApJ. 646 (2006) 1303, ibid. 595 (2003) 1277

Hathaway, http://science.msfc.nasa.gov/ssl/pad/solar/quests.html (2003) http://science.nasa.gov/headlines/y2002/06feb hessi.htm

The Mysterious Origins of Solar Flares

What produces solar flaresWhat produces solar flares? ? μflares, nanoflares,.., CMEs

flare-quiet ≈≈ flare-imminent regions… storage and release of the energy that powers solar flares

is generally believedbelieved to be in the coronal magnetic field …

What ignites solar flares?How do they unleash so much energy so quickly?

GD Holman, SCIENTIFIC AMERICAN, April 2006

41

~ 15-20MK

The Electron “Problem”e- ≈ 105× hard X-raysfrom Bremsstrahlung!

FLARES

Rebinned peak flare X-ray intensity Bmax

Mason et al., ApJ. 645 (2006) 1543 B2 correlation

Lx↑

Bmax

G. Emslie (2005)http://www.astro.auth.gr/%7Evlahos/ascona/memberstalks/energeticsEmslie.ppt#366,8

surface brightness < maximum Laxion

Lx ∝ B2

42

Brightening:Disk Centreoutside DC

43

Search for solar X-rays from axions

Soft X-rays from Hinode/Yohkoh showing an axion signal. The axions, for a uniform coronal magnetic field,would give an image of the solar core.

simulation

RHESSIscience nuggetH. Hudson,30.4.2007

~2.5 days crossing time brightening

44

Sunspot counts

Carlson & Tseng,Phys. Lett. B365 (1996) 193

CAST in SunspotsCAST in Sunspots??““ Unfortunately, the signal is dominated byUnfortunately, the signal is dominated by background background XX--ray emission from sunspots as they cross the DC of the Sun ray emission from sunspots as they cross the DC of the Sun

a brightening ~2.5a brightening ~2.5 days!days!

coun

ts/s

×× Rsolar~2××1.4 daysCrossing time

45

Yohkoh

11 May 1998 07:50:31 UT3

Crossing disk centreCrossing disk centre

Flares

Yohkoh /SXT

X-Ray Bright Point @ Solar Disk Centre ~2.5 d

Start Time 10 May 1998_00:00

??Smallest event:

~1 % of classical ARs

Mandrini et al., A&A 434(2005)725L. vanDriel-Gesztelyi,private communication

CrossingCrossing disk centre,disk centre, 1.8oN

more?

Thanks!Th. Papaevangelou

Alternative search @ other energies/places?

Motivation:Motivation: the ~2MK hot corona!

< a few 100< a few 100 eVeV soft X-rays

e.g. data from:e.g. data from: YohkohYohkohHinodeHinodeSOHO SOHO EVE EVE 2008-CASTCAST

48

If g & m of an ALP depend on temperature and density:

suppression of production in stellar plasmas

relaxed astrophysical boundsJaeckel, Masso, Redondo, Ringwald, Takahashi, PR D75 (2007) 013004

Anomaly induced effects in a magnetic field… modification of QED by a light massive vector field mB< 1eV …

very similar to… ALPs...including millicharged fermionsmΨ ~ 1eV–1keV

the production of the new vector field is suppressed @ high energies by

~(mB/kTcore)2 ~ 10-6avoid stellar bounds + bounds from CMB

Antoniadis, Boyarsky, Ruchayskiy, CERN-PH-TH/2007-135, hep-ph/0708.3001 22 Aug 2007

Bounds for ~axions from solar/stellar evolution, but …

49

Solar activity near equator!

50

Longitude + + latitude positions of ~24000 μflares

http://sprg.ssl.berkeley.edu/~tohban/nuggets/?page=article&article_id=52

20/5/2007, RHESSI nuggetHannah, Christe

Magnetic flux ~95% in ±40o R. Howard, Sol Phys 38(1974)59

Song, Feng, Hu, ApJL. 667 (Sept. 2007)

52

Å

Benevolenskaya, Kosovichev, Lemen, Scherrer, Slater ApJ. 571 (2002) L181

Latitu

de/d

eg

Latitu

de/d

egEUVEUV

5-12 Å (

Look @ very quiet Sun YOHKOHYOHKOH//XRTXRT49 days

V.Anastassopoulos, M.Tsagri

54

Energy deposition/#

V.Anastassopoulos, M.Tsagri

Histogram of pixel values (distribution of gray levels) for the image corresponding to the simple summation of all (66) sun images in solar maximum (1999-2000). The maximum pixel value of 16830 is normalized to 255.

Solar MaximumYOHKOH

Thanks S.Orlando

Energy deposition/#

Histogram of pixel values (distribution of gray levels) for the image corresponding to the simple summation of all (49) quiet sun images from year 1996.The maximum pixel value of 12495 is normalized to 255.

Solar Minimum

55

Summation of all pixels of the quiet images with values 7-35.

Summation of all pixels of the quiet images with values 7-35.

Solar Minimum Solar MaximumYOHKOH

V.Anastassopoulos, M.Tsagri56

V.Anastassopoulos, M.Tsagri

The equalized image in pseudo-color.The equalized image in pseudo-color.

Solar MaximumSolar MinimumYOHKOH

57

ν’s

Cycles / year

SXT S60SXT S60oo N60N60oo

58

SXT equatorSXT equator

GALLEXGALLEX

Caldwell, Sturrock, Astroparticle Phys. 23 (2005) 543Weber, Sturrock, Yohkoh 10th Anniversary Meeting, COSPAR Coll. Ser. 13 (2002) 323,347

X-rays Yohkoh

HomestakeHomestake

~0.7R⊙⊙ ~0.8R⊙⊙

overshoot layerovershoot layer??additional heatingadditional heating?

S Solanki,private communication

SunSun--ModelModel // SunSun

tachocline

The solar internal sound speed

~2~2MKMK

Helioseismology

~100T 1 T

Hiremath, Lovely ApJ. 667 (20.9.2007) 58559

• 11 years cycle• Solar corona heating problem• B⊙• Sunspots heat flux problem11• Flares instantaneous particle acceleration• Solar metallicity

Open solar questions

60

Ne/O abundance ratios vs. coronal activity.

measured photospheric abundances ofC,N,O,Ne 25-35% below prediction!

M. Asplund et al., astro-ph/200410214 :

Drake, Testa, Nature 436 (2005) 525

61

Solar models constructed with the new, low abundancesare incompatible with the helioseismic observations.

. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . The Solar Model problemThe Solar Model problem

Terrible for solar modelingTerrible for solar modeling

The Solar Oxygen crisisThe Solar Oxygen crisis

FFind a truly solarind a truly solar--like starlike starwhy the Sun is so special ?why the Sun is so special ?

"non-standard" physical processes …

Liefke, Schmitt, A&A L. (2006) ; Basu et al., ApJ. 655 (2006) 660 IAU General Assembly Meeting, Prague, August 14 - 25, 2006

Asplund, Grevesse, Güdel, Sauval, astro-ph/200510377Montalban, Miglio, Theado, Noels, Grevesse,

http://www.astro.ulg.ac.be/RPub/Colloques/JENAM/proceedings/asterosis/Montalban.pdf62

Abundance ratios, 30 min running averages of 5 min data from CELIAS/MTOF - SOHO. Raymond et al., CP598, Solar and Galactic Composition, ed. Wimmer-Schweingruber A I P (2001) 49

… vary from place to place + + time to time.

Solar elemental abundances …

Solar Solar axionaxion surface effects at worksurface effects at work??

… changing diffusion locally.

Martin Asplund, private communication, 11/9/2006

64

Differential radiation pressure

s. Schmelz et al., ApJ.634 (2005) L197,+ Shemi, MNRAS 251 (1991) 221; Young, astro-ph/200510264

Flares: e.g.: Ne:O ≈ 0.42 in SEPs & variations of ~2× observed stars more active!

Quiet ARs,quiet Sun:Ne / O at ~0.15. The “Solar Model problem” !

Axion scenario:

• Outwards pressure ( B ) more Neon

• Inwards pressure ( self-irradiation) less Neon

Note:Note: σpe(Ne-to-O) > 2× at Eγ~1 keV

Thanks A.Nordt

65

Solar oxygen abundance B at the base of the photosphere near a porepore. The blue line: B2-dependence + constant component

H. Socas-Navarro, Private Comunication.

Z., Semertzidis, Papaevangelou, astro-ph/200701627

Oxygen abundanceOxygen abundance

B2

Fit B2.12±0.27

66

Photons survive (dashed line) with an enhancement factor ~20 as expected in the absence of an a-γ oscillation: ma«10-10eV, gaγγ220 GeV ++ z=0.54 is unexpected.De Angelis, private communication

””New PhysicsNew Physics””Large transparency to extragalactic light

Quasar Quasar 3C2793C279z=0.54

without oscillation

with axion-γ oscillation

MAGIC Telescope: Obs’d VHE γ’s >220 GeV 5.1σ30th ICRC’07, Merida, Mexico

astro-ph/0709.1475, 10/9/2007

67

Day, Phys. Today (2003) 16; Peng Oh, MNRAS 353 (2004) 468; Ikebe, Böhringer, Kitayama, ApJ. 611 (2004) 175; Nadis, Astronomy 33 (2005) 34; Demarco, Rosati, Ford, Modern Phys. Lett. A20 (2005) 1409; Cavalieri, Lapi, Rephaeli, ApJ. 634 (2005) 784, Lyutikov, astro-ph/0709.1712 ApJL 2007

Lx ∝ Tx2 (1+z)3/2 expected

Lx ∝ Tx3 observed + decreasing with z!

some thing non-gravitational is heating the gas again!A key problem of ICMabsence of strong cooling @ the centre of GCs

details of the heating process remain mysterious. mysterious.

The source(s) of the ““excessexcess”” entropyentropy? entropy floor problem

a ~30 years-long-standing puzzle

““additionaladditional”” gas physicsgas physics??

Galaxy ClustersGalaxy Clusters

68

2.72.7 K K CMBCMB

BEFORE

AFTERAFTER

CMB:CMB:

SunyaevSunyaev -- ZelZel’’dovichdovich (SZ) effect(SZ) effect

Galaxy ClusterGalaxy Cluster

AFTERAFTERBEFOREBEFORECMB:CMB:

• Scattering of CMB off hot electrons in the ICM: σcompton ~ ρe• Probes the thermal energy distribution of electrons in the ICM.

• SZ flux is redshift independent: ~ ρexTea) NOT contamination of radio sourcesb) X-rays, only from Bremsstrahlung? ? ΦX-rays ~(ρe)²² x (Te)1/21/2

+ radiatively decaying ~axions?Decay rDecay rate ~ρaxion

Z., Z., DennerlDennerl, Hoffmann, , Hoffmann, PapaevangelouPapaevangelou SCIENCE 306 (SCIENCE 306 (2004) 1485 ) 1485 LaBoqueLaBoque et al., et al., ApJApJ. 652 (. 652 (2006) 917) 917

ghost plasmaghost plasma

69

Observed integrated gas mass fractions = f(overdensity ∆) [left] within ∆=1500 of the ICM [right]. Chandra & & XMM-Newton

McCarthy, Bower, Balogh, MNRAS 377 (20072007) 1457

Galaxy Clusters Galaxy Clusters WMAPWMAP__3years

70

Galaxy ClusterGalaxy Cluster

Afshordi, Lin, Nagai, Sanderson, MNRAS 378 (2007) 293, Afshordi, New Astron. Rev. 50 (2006) 905Bielby, Shanks, astro-ph/0703470, MNRS (2007).

One of the most surprising findings:One of the most surprising findings:

Anomalous (=overpredicted) SZ 3 Year WMAP3 Year WMAP

~30~30--40%40% of the baryons is missing in ICM both in SZ+WMAP.

Missing Baryons or Missing Baryons or New AstrophysicsNew Astrophysics??. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

e.g.:e.g.:

Z., Z., DennerlDennerl, Hoffmann, , Hoffmann, PapaevangelouPapaevangelou SCIENCE 306 (SCIENCE 306 (2004) 1485) 1485

Or, decaying massive ~axions??

71

Origin of diffuse X-rays?

too hot (~ 90MK) to be a gravitationally bound plasma!

how to produce it?

Galactic Center

72

In conclusion:In conclusion:

73

In conclusion:In conclusion:

Persisting astrophysical problems suggest new physics

74

THANK YOUTHANK YOU!!

76

The Primakoff Effect 1951