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
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
