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Page 1: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Puzzles of Dark Matter Searches - a signature for Composite Dark Matter?

Presented to Seminar in ULB, 13.04.2010

Page 2: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Outlines• Puzzles of Direct Dark matter searches • Physical reasons for new stable quarks and/or

leptons• Exotic forms of composite dark matter, their

cosmological evolution and effects in underground detectors

• Cosmic-ray and accelerator search for charged components of composite dark matter

Page 3: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Dark Matter – Cosmological Reflection of Microworld Structure

Dark Matter should be present in the modern Universe, and thus is stable on cosmological scale.

This stabilty reflects some Conservation Law, which prohibits DM decay.

Following Noether’s theorem this cosnservation law should correspond to a (nearly) strict symmetry of microworld.

Page 4: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

4

DDirect search for DM (WIMPs)irect search for DM (WIMPs)

DM can consist of Weakly Interacting Massive Particles (WIMPs).

Such particles can be searched by effects of WIMP-nucleus interactions.

2222

maxmax 2

2

20 vm

m

v

m

qTT Amm

AAAX

keV10~,s

km300~ Tv

1(max)

*max

A

A

Rq

ET elastic scattering

non-pointlike nucleus

)( 2point qFAAamplitudenInteractio AAXAX

Page 5: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

5

DDirect search for DM (WIMPs)irect search for DM (WIMPs)

Minimization of background

• Installation deeply underground

• Radioactively pure materials

• Annual modulation

DM does not participate in rotation around GC.

%7~232

15~

cos~

June2

)km/s(53sin25cos5.16220

)(coscos

0

0

ySun

orb

ySun

orbySunyEarth

v

vAmplitude

t

v

ttvvv

Page 6: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

6

DDirect search for DM (WIMPs)irect search for DM (WIMPs)

.3.6

cpd/kg/keV)3(020.0

year010001

days22May210

levelConfedence

Amplitude

..T

t

Experiment DAMA (NaI)

Results of 7 years of observation (1995-2002).DAMA/NaI (7 years) + DAMA/LIBRA (4 years) total exposure: 300555 kgday = 0.82

tonyr

00 cos)( ttSStR m

8.3s138 ±70.996 ±0.0020.0223 ±0.0027(2÷4) keV

DAMA/NaI + DAMA/LIBRA

DAMA/LIBRA (4 years)

6.7s139 ±100.997 ±0.0020.0213 ±0.0032(2÷4) keV

6.9s143 ±90.998 ±0.0020.0165 ±0.0024(2÷5) keV

5.6s144 ±110.998 ±0.0030.0107 ±0.0019(2÷6) keV

5.5s140 ±301.01 ±0.020.0215 ±0.0039(2÷5) keV

5.0s125 ±301.01 ±0.020.0252 ±0.0050(2÷4) keV

DAMA/NaI (7 years)

144 ±8

145 ±7

140 ±22

t0 (day)

8.2s0.998 ±0.0030.0131 ±0.0016(2÷6) keV

8.9s0.998 ±0.0020.0178 ±0.0020(2÷5) keV

6.3s1.00 ±0.010.0200 ±0.0032(2÷6) keV

C.L.T=2p/? (yr)A (cpd/kg/keV)

8.3s138 ±70.996 ±0.0020.0223 ±0.0027(2÷4) keV

DAMA/NaI + DAMA/LIBRA

DAMA/LIBRA (4 years)

6.7s139 ±100.997 ±0.0020.0213 ±0.0032(2÷4) keV

6.9s143 ±90.998 ±0.0020.0165 ±0.0024(2÷5) keV

5.6s144 ±110.998 ±0.0030.0107 ±0.0019(2÷6) keV

5.5s140 ±301.01 ±0.020.0215 ±0.0039(2÷5) keV

5.0s125 ±301.01 ±0.020.0252 ±0.0050(2÷4) keV

DAMA/NaI (7 years)

144 ±8

145 ±7

140 ±22

t0 (day)

8.2s0.998 ±0.0030.0131 ±0.0016(2÷6) keV

8.9s0.998 ±0.0020.0178 ±0.0020(2÷5) keV

6.3s1.00 ±0.010.0200 ±0.0032(2÷6) keV

C.L.T=2p/? (yr)A (cpd/kg/keV)

Page 7: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

7

OtherOther search searcheses for DM (WIMPs) for DM (WIMPs)

Experiment DAMA (NaI) vs other underground experiments:Interpretation in terms of scalar AX-interaction.

Analysis depends essentially on assumption about distribution of DM in vicinity of Solar system. On this picture a quite simplified assumption was adopted.

DAMA(NaI) under variety of assumptions

Experiment DAMA/NaI+DAMA/Libra vs other underground experiments:

arXive: 0808.3607 [astro-ph]0912.3592

two events were observed; the probability of observing two or more background events is 23%

Minimal SUSY model predictions

Page 8: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

8

DDirect search for DM (irect search for DM (SDI SDI WIMPs)WIMPs)

Experiment DAMA (NaI) vs other underground experiments:Interpretation in terms of spin-spin AX-interaction.

Experiment DAMA/NaI+DAMA/Libra vs other underground experiments:

Super-Kamiokande (see slides 11-15)

Page 9: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

9

DDirect search for DM (SIMPs)irect search for DM (SIMPs)

Rocket experiment XQC.

If DM consists of Strongly Interacting Massive Particles (SIMPs), they could be slowed down by ordinary matter and become insensitive for underground detectors.

Such particles could be searched for in X-cosmic ray experiment XQC, aimed at observation of X-rays and realized during a rocket flight.

XQC experiment

data taking time: ~100s,

material of detector: Si+HgTe,

energy deposit range of sensitivity: 25-1000 eV,

the range being good for extraction of SIMP-nucleus interactions event from background: 25-60 eV.

For scalar XA-interaction

Page 10: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Dark Matter from Charged Particles?

2

PlPl

mM m

m

• However, if charged particles are heavy, stable and bound within neutral « atomic » states they can play the role of composite Dark matter.

• Physical models, underlying such scenarios, their problems and nontrivial solutions as well as the possibilities for their test are the subject of the present talk.

By definition Dark Matter is non-luminous, while charged particles are the source of electromagnetic radiation. Therefore, neutral weakly interacting elementary particles are usually considered as Dark Matter candidates. If such neutral particles with mass m are stable, they freeze out in early Universe and form structure of inhomogeneities with the minimal characterstic scale

Page 11: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Components of composite dark matter:

• Tera-fermions E and U of S.L.Glashow’sTera-fermions E and U of S.L.Glashow’s

• Stable U-quark of 4-th familyStable U-quark of 4-th family

• AC « leptons » from almost commutative AC « leptons » from almost commutative geometrygeometry

• Technibaryons and technileptons from Technibaryons and technileptons from Walking Technicolor (WTC)Walking Technicolor (WTC)

•Stable U-quarks of 5th family in the Stable U-quarks of 5th family in the approach, unifying spins and charges, by approach, unifying spins and charges, by N. Mankoc-BorstnikN. Mankoc-Borstnik

Page 12: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.
Page 13: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.
Page 14: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Glashow’s tera-fermions

E

N

D

U

Very heavy and unstableVery heavy and unstable

m~500 m~500 GeVGeV, , stablestable

m~3 m~3 TeVTeV, , ((metameta))stablestable

m~5 m~5 TeVTeV, D , D U +… U +…

SU(3)xSU(2)xSU(2)xU(1)SU(3)xSU(2)xSU(2)xU(1)

Tera-fermionsTera-fermions ((N,E,U,DN,E,U,D) ) W’, W’, Z’Z’, , H’, H’, and g and g

101066

++ problem of CP-violation in QCDproblem of CP-violation in QCD ++ problem of neutrino problem of neutrino massmass

++ (?) (?) DM DM asas [(UUU)EE] tera-helium [(UUU)EE] tera-helium (NO!)(NO!)

6

vev

vevUE D

e u d

mm mS

m m m

Page 15: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.
Page 16: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Cosmological tera-fermion asymmetry

( ) 0.224UUUEE CDM

0.044b

• To saturate the observed dark matter of the Universe Glashow assumed tera-U-quark and tera-electron excess generated in the early Universe.

• The model assumes tera-fermion asymmetry of the Universe, which should be generated together with the observed baryon (and lepton) asymmetry

However, this asymmetry can not suppress primordial antiparticles, as

it is the case for antibaryons due to baryon asymmetry

Page 17: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.
Page 18: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.
Page 19: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.
Page 20: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.
Page 21: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.
Page 22: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

(Ep) catalyzer

• In the expanding Universe no binding or annihilation is complete. Significant fraction of products of incomplete burning remains. In Sinister model they are: (UUU), (UUu), (Uud), [(UUU)E], [(UUu)E], [(Uud)E], as well as tera-positrons and tera-antibaryons

• Glashow’s hope was that at T<25keV all free E bind with protons and (Ep) « atom » plays the role of catalyzer, eliminating all these free species, in reactions like

pEEEpE

pEEUUUEpEUUU

][][

But this hope can not be realized, since much earlier all the free E are trapped by He

Page 23: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.
Page 24: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

« No go theorem » for -1 charge components

• If composite dark matter particles are « atoms », binding If composite dark matter particles are « atoms », binding positive P and negative E charges, all the free primordial positive P and negative E charges, all the free primordial negative charges E bind with He-4, as soon as helium is negative charges E bind with He-4, as soon as helium is created in SBBN.created in SBBN.

• Particles E with electric charge -1 form +1 ion [E He]Particles E with electric charge -1 form +1 ion [E He]..

• This ion is a form of anomalous hydrogenThis ion is a form of anomalous hydrogen..

• Its Coulomb barrier prevents effective binding of positively charged particles P with E. These positively charged particles, bound with electrons, become atoms of anomalous istotopes

• Positively charged ion is not formed, if negatively charged Positively charged ion is not formed, if negatively charged particles E have electric charge -2.particles E have electric charge -2.

Page 25: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

4th family from heterotic string phenomenology

• 4th family can follow from heterotic string phenomenology as naturally as SUSY.• GUT group has rank (number of conserved quantities) 6, while SM, which it

must embed, has rank 4. This difference means that new conserved quantities can exist.

• Euler characterics of compact manifold (or orbifold) defines the number of fermion families. This number can be 3, but it also can be 4.

• The difference of the 4th family from the 3 known light generations can be explained by the new conserved quantity, which 4th generation fermions possess.

• If this new quantum number is strictly conserved, the lightest fermion of the 4th generation (4th neutrino, N) should be absolutely stable.

• The next-to-lightest fermion (which is assumed to be U-quark) can decay to N owing to GUT interaction and can have life time, exceeding the age of the Universe.

• If baryon asymmetry in 4th family has negative sign and the excess of anti-U quarks with charge -2/3 is generated in early Universe, composite dark matter from 4th generation can exist and dominate in large scale structure formation.

6E

Page 26: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

4-th family

E

N

D

U

m~50 m~50 GeVGeV, (, (quasiquasi))stablestable

100 100 GeVGeV <m<~1<m<~1 TeVTeV, E ->N l, E ->N l,…,… unstableunstable

220 220 GeVGeV <m<~1<m<~1 TeVTeV, U ->, U -> N + light fermions Long-N + light fermions Long-living wihout mixing with light generationsliving wihout mixing with light generations

220 220 GeVGeV <m<~1<m<~1 TeVTeV, D ->, D -> U lU l,… unstable,… unstable

Precision measurements of SM parameters admit existence of 4th family, if 4th neutrino has mass around 50 GeV and masses of E, U and D are near their experimental bounds.

If U-quark has lifetime, exceeding the age of the Universe, and in the early Universe excess of anti-U quarks is generated, primordial U-matter in the form of ANti-U-Tripple-Ions of Unknown Matter (anutium). UUU UUU can become a -2 charge constituent of composite

dark matter4th neutrino with mass 50 GeV can not be dominant form of dark matter. But even its sparse dark matter component can help to resolve the puzzles of direct and indirect WIMP searches.

Page 27: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

4UUU He UUU He

But it goes only after He is formed at T ~100 keV

131/ 2 10o He HeR ZZ m cm

The size of O-helium is

2 2 2 1.6o He HeI Z Z m MeV

It catalyzes exponential suppression of all the remaining U-baryons with positive charge and causes new types of nuclear transformations

Dominant form of 4th generation dark matter: O-helium formation

0IT

Page 28: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

O-Helium: alpha particle with zero charge

• O-helium looks like an alpha particle with shielded electric charge. It can closely approach nuclei due to the absence of a Coulomb barrier. For this reason, in the presence of O-helium, the character of SBBN processes can change drastically.

• This transformation can take place if

, 4, 2A Z UUU He A Z UUU

, 4, 2He oM A Z m I M A Z This condition is not valid for stable nuclids, participating in SBBN processes, but unstable tritium gives rise to a chain of O-helium catalyzed nuclear reactions towards heavy nuclides.

Page 29: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

OHe catalysis of heavy element production in SBBN

Page 30: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

OHe induced tree of transitions

After K-39 the chain of transformations starts to create unstable isotopes and gives rise to an extensive tree of transitions along the table of nuclides

Page 31: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Complicated set of problems

• Successive works by Pospelov (2006) and Kohri, Takayama (2006) revealed the uncertainties even in the roots of this tree.

• The « Bohr orbit » value is claimed as good approximation by Kohri, Takayama, while Pospelov offers reduced value for this binding energy. Then the tree, starting from D is possible.

• The self-consistent treatment assumes the framework, much more complicated, than in SBBN. Nuclear physics of OHe reactions should be evolved

2 2 2 1.6o He HeI Z Z m MeV

Page 32: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Sunod

PlPl

od

RMod M

T

mm

T

TM 9

2

10

O-helium dark matter

• Energy and momentum transfer from baryons to O-helium is not effective and O-helium gas decouples from plasma and radiation

• O-helium dark matter starts to dominate

• On scales, smaller than this scale composite nature of O-helium results in suppression of density fluctuations, making O-helium gas more close to warm dark matter

1b p on v m m t

keVTT od 1

eVTRM 1

Page 33: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Anutium component of cosmic rays

• Galactic cosmic rays destroy O-helium. This can lead to appearance of a free anutium component in cosmic rays.

Such flux can be accessible to PAMELA and AMS-02 experiments

7104

He

UUU

Page 34: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Rigidity of Anutium component

Difference in rigidity provides discrimination of U-helium and nuclear component

Page 35: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

O-helium in Earth

• Elastic scattering dominates in the (OHe)-nucleus interaction. After they fall down terrestrial surface the in-falling OHe particles are effectively slowed down due to elastic collisions with the matter. Then they drift, sinking down towards the center of the Earth with velocity

Page 36: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

O-helium experimental search?

• In underground detectors, (OHe) “atoms” are slowed down to thermal energies far below the threshold for direct dark matter detection. However, (OHe) nuclear reactions can result in observable effects.

• O-helium gives rise to less than 0.1 of expected background events in XQC experiment, thus avoiding severe constraints on Strongly Interacting Massive Particles (SIMPs), obtained from the results of this experiment.

It implies development of specific strategy for direct experimental search for O-helium.

Page 37: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Superfluid He-3 search for O-helium

• Superfluid He-3 detectors are sensitive to energy release above 1 keV. If not slowed down in atmosphere O-helium from halo, falling down the Earth, causes energy release of 6 keV.

• Even a few g existing device in CRTBT-Grenoble can be sensitive and exclude heavy O-helium, leaving an allowed range of U-quark masses, accessible to search in cosmic rays and at LHC and Tevatron

Page 38: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

O-helium concentration in EarthThe O-helium abundance the Earth is determined by the equilibrium between the in-falling and down-drifting fluxes.

The in-falling O-helium flux from dark matter halo is

where Vh is velocity of Solar System relative to DM halo (220 km/s), VE is velocity of orbital motion of Earth (29.5 km/s) and

is the local density of O-helium dark matter. At a depth L below the Earth's surface, the drift timescale is ~L/V. It means that the change of the incoming flux, caused by the

motion of the Earth along its orbit, should lead at the depth L ~ 105 cm to the corresponding change in the equilibrium underground concentration of OHe on the timescale

Page 39: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Annual modulation of O-helium concentration in Earth

The equilibrium concentration, which is established in the matter of

underground detectors, is given by

where T=1yr and to is the phase. The averaged concentration is given by

and the annual modulation of OHe concentration is characterized by

The rate of nuclear reactions of OHe with nuclei is proportional to the local concentration and the energy release in these reactions leads to ionization signal containing both constant part and annual modulation.

Page 40: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

OHe solution for puzzles of direct DM search

• OHe equilibrium concentration in the matter of DAMA detector is maintained for less than an hour

• The process

is possible, in which only a few keV energy is released. Other inelastic processes are suppressed

• Annual modulations in inelastic processes, induced by OHe in matter. No signal of WIMP-like recoil

• Signal in DAMA detector is not accompanied by processes with large energy release. This signal corresponds to a formation of anomalous isotopes with binding energy of few keV

ZAOHeZAOHe ,),(

Page 41: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Formation of OHe-nucleus bound system

r

V

OHe

Due to exponential tail of nuclear Yukawa force OHe is attracted by nucleus. At the distance of order of the size of OHe Coulomb barrier is switched on. If He emits a photon, OHe forms a bound system with nucleus with binding energy of few KeV.

oA rR

31

ARA AgA The depth of the well is maximal for A~10-20

AR

E~few keV

Vcul=

Vnuc=

Page 42: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Few keV Level in OHe-nucleus system in NaI

• The problem is reduced to a quantum mechanical problem of finding energy level of OHe bound state in the spherically symmetric potential well, formed by Yukawa attraction and Coulomb barrier for He nucleus component of OHe in vicinity of a nucleus.

• The numerical solution for this problem is simplified for rectangular wells and walls, giving a few keV level for Na and I .

Page 43: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Few keV Levels in OHe-Na and OHe-I systems

Page 44: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Levels in OHe-Ge system

Page 45: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Levels in OHe-Xe system

Page 46: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Rate of OHe-nucleus radiative capture

As soon as the energy of level is found one can use the analogy with radiative capture of neutron by proton with the account for:

• Absence of M1 transition for OHe-nucleus system (which is dominant for n+p reaction)

• Suppression of E1 transition by factor f~10-3, corresponding to isospin symmetry breaking

(in the case of OHe only isoscalar transition is possible, while E1 goes due to isovector transition only)

Page 47: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Reproduction of DAMA/NaI and DAMA/LIBRA events

The rate of OHe radiative capture by nucleus with charge Z and atomic number A to the energy level E in the medium with temperature T is given by

Formation of OHe-nucleus bound system leads to energy release of its binding energy, detected as ionization signal. In the context of our approach the existence of annual modulations of this signal in the range 2-6 keV and absence of such effect at energies above 6 keV means that binding energy of Na-OHe and I-OHe systems in DAMA experiment should not exceed 6 keV, being in the range 2-4 keV for at least one of these elements.

Page 48: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Annual modulation of signals in DAMA/NaI and DAMA/LIBRA events

The amplitude of annual modulation of ionization signal

(measured in counts per day per kg, cpd/kg) is given by

Page 49: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Rates of OHe capture in other detectorsSince OHe capture rate is proportional to the temperature, it should be suppressed in cryogenic detectors. However, for the size of cryogenic devices less, than few tens meters, OHe gas in them has the temperature of the surrounding matter and the suppression relative to room temperature is only ~mA/mo.

Content Binding energy(keV)

Capture rate(10-30 cm3/s)

Counts per day(10-3 cpd/kg)

Ge (CDMS)

8.6 5 7.3

Ge(CoGeNT)

8.6 0.037 55

Xe 6.1 0.14 11.6

Ar 15.6 4.3 11.4

C 398.5 0.15 1.4

Page 50: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Excessive positrons in IntegralTaking into account that in the galactic bulge with radius 1 kpc the ∼

number density of O-helium can reach the value

one can estimate the collision rate of O-helium in this central region:

At the velocity of particules in halo, energy transfer in such collisions is E 1MeV. These collisions can lead to excitation of O-helium. If 2S ∼level is excited, pair production dominates over two-photon channel in the de-excitation by E0 transition and positron production with the rate

is not accompanied by strong gamma signal. This rate of positron production is sufficient to explain the excess of positron production in bulge, measured by Integral.

Page 51: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Gamma lines from bulge

• If OHe levels with nonzero orbital momentum are excited, gamma lines should be observed from the transitions

at the level

Page 52: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

O-helium Universe?

• The proposed scenario is the minimal for composite dark matter. It assumes only the existence of a heavy stable U-quark and of an anti-U excess generated in the early Universe to saturate the modern dark matter density. Most of its signatures are determined by the nontrivial application of known physics. It might be too simple and too pronounced to be real. With respect to nuclear transformations, O-helium looks like the “philosopher’s stone,” the alchemist’s dream. That might be the main reason why it cannot exist.

• However, its exciting properties put us in mind of Voltaire: “Se O-helium n’existai pas, il faudrai l’inventer.”

Page 53: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

More Examples: AC-model

Mass of AC-leptons has « geometric origin ». Experimental constraint We take m=100GeV Their charge is not fixed and is chosen +-2 from the above cosmological arguments. Their absolute stability can be protected by a strictly conserved new U(1) charge, which

they possess.In the early Universe formation of AC-atoms is inevitably accompanied by a fraction of

charged leptons, remaining free.

100A Cm m m GeV

++ follows from unification of General Relativity and gauge follows from unification of General Relativity and gauge symmetries on the basis of almost commutative (AC) geometry symmetries on the basis of almost commutative (AC) geometry (Alain Connes)(Alain Connes)

++ DM DM ((AC ) “atoms”AC ) “atoms”

Extension of Standard model by two new doubly charged « leptons »Extension of Standard model by two new doubly charged « leptons »

They are leptons, since they possess only They are leptons, since they possess only and Z (and new, y-) and Z (and new, y-) interactions interactions

2S

Form neutral atoms (AC, O-helium,….)-> composite dark matter Form neutral atoms (AC, O-helium,….)-> composite dark matter candidates!candidates!

Page 54: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

More Examples: WTC-model

The ideas of Technicolor are revived with the use of SU(2) group for “walking” (not running ) TC gauge constant. U and D techniquarks transform under the adjoint representation of an SU(2) technicolor gauge group. The chiral condensate of the techniquarks breaks the electroweak symmetry. There are nine Goldstone bosons emerging from the symmetry breaking. Three of them are eaten by the W and the Z bosons. The remaining six Goldstone bosons (UU, UD, DD and their corresponding antiparticles) are technibaryons and corresponding anti-technibaryons. The electric charges of UU, UD, and DD are given in general by y+1, y, and y-1 respectively, where y is an arbitrary real number.To cancel the Witten global anomaly model requires in addition the existence of a fourth family of leptons ( and ). Their electric charges are in terms of y respectively (1 - 3y)/2 and (-1 - 3y)/2.

Page 55: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Charged techniparticles

• If y=1, and UU is the lightest it has charge +2, while its stable antiparticle has charge -2.

• In addition for y = 1, the electric charges of and are respectively -1 and -2.

• If TB is conserved, is main constituent of composite dark matter.

• If L’ is conserved, composite dark matter is provided by

• Their mixture if both the technilepton number L’ and are TB conserved.

Page 56: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Techniparticle excess

• The advantage of WTC framework is that it provides definite relationship between baryon asymmetry and techniparticle excess.

Here are statistical factors in equilibrium relationship between, TB, B, L and L’

The equilibrium is maintained by electroweak SU(2) sphalerons and similar relationship can hold true for any SU(2) dublets (like U quarks of 4th family or stable quarks of 5th family)

Page 57: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Relationship between TB and B

• L’=0, T*=150 GeV

=0.1; 1; 4/3; 2; 3

• L’=0, T*=150, 200, 250 GeV

Page 58: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Relationship between TB, L’ and B

• x denotes the fraction of dark matter given by the technibaryon

• TB<0, L’>0 – two types of -2 charged techniparticles.

The case TB>0, L’>0 (TB<0, L’<0 ) gives an interesting possibility of (-2 +2) atom-like WIMPs, similar to AC model. For TB>L’ (TB<L’) no problem of free +2 charges

Page 59: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

A WTC Universe?

• Even minimal, WTC model gives a wide variety of possibilities for composite dark matter scenario.

• It provides relationship between baryon asymmetry and dark matter.

• It makes possible nearly WDM (techni-O-helium) or mixed WDM+CDM scenarios

• Techni-O-helium is necessary (and even dominant) element of such scenarios

Page 60: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

A solution for cosmic positron excess?

• If both technibaryons UU and technileptons are present, CDMS results constrain WIMP-like (UU ) component to contribute no more than 1% of total DM density.

• Decays of positively charged UU->e+ e + with a lifetime of about and mass 300-400 GeV can explain the excess of cosmic positrons, observed by PAMELA

s2410

Page 61: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Invisble decay of Higgs bosonInvisble decay of Higgs boson H H ->-> NNNN

Search for unstable quarks and Search for unstable quarks and leptons of new families are well leptons of new families are well elaboratedelaborated..

Search for stable particles at LHC

Page 62: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Expected mass spectrum of U hadronsMesons

Baryons

Uud

dU~ 0~uU

MU

+0.2

+0.4

+0.6

GeV

sU~

Usu 0Usd

Uud Uuu Udd

,l

e

)( U

)( 0/M

The same for U-hadrons

Uud

0~uU duU ~~~

dU~ dU~

sU~

sU~

0/~~~ qsU

0/Usq

0~uU

8%

40%

40%

12%

~1%

Yields of U-hadrons in ATLAS

Page 63: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Possible signature of stable U hadrons Particle transformation during propagation

through the detector material

This signature is substantially different from that of R-hadrons

S. Helman, D. Milstead, M. Ramstedt, ATL-COM-PHYS-2005-065

Muon detector

ID&EC&HC

U-hadron does not change charge (+) after 1-3 nuclear interaction lengths (being in form of baryon)

U-hadron changes its charge (0-) during propagation through the detectors (being in form of meson)

/0/0 ~~MM

UU UM /0

/0~~MU

,...~~ /0 MNU

,...~~ /0/0 NMNM

,...~

NNU

,.../0 NNMNU

,.../0/0 NMNM

,... U

sU~ UsuUsd 0

U-baryon will be converted into U-meson

U-mesons will experience inter-conversion

U-baryon will not be converted

U-mesons will experience inter-conversion and convert to U-baryon

Strange U-hadrons will get the form

and

suppressed

suppressed

“+” - 60%

“0” - 40%

“-” - 60%

“0” - 40%

Page 64: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

LHC discovery potential for components of composite dark matter

• In the context of composite dark matter search for new (meta)stable quarks and leptons acquires the meaning of crucial test for its basic constituents

• The level of abscissa axis corresponds to the minimal level of LHC sensitivity during 2 years of operation

Page 65: Puzzles of Dark Matter Searches - a signature for Composite Dark Matter? Presented to Seminar in ULB, 13.04.2010.

Conclusions• New stable quarks and leptons can appear in extensions of Standard Model.

•Composite dark matter and its basic constituents are not excluded either by experimental, or by cosmological arguments and are the challenge for cosmic ray and accelerator search

• Small fraction or even dominant part of composite dark matter can be in the form of O-helium, catalyzing new form of nuclear transformation

• The test for composite dark matter is possible in cosmoparticle physics analysis of its signatures and experimental search for stable charged particles in cosmic rays and at accelerators.