Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://master.sai.msu.ru/static/YaB_100/20/Khlopov.pdf Äàòà èçìåíåíèÿ: Tue Apr 8 19:44:20 2014 Äàòà èíäåêñèðîâàíèÿ: Sat Apr 9 23:34:41 2016 Êîäèðîâêà: Ïîèñêîâûå ñëîâà: ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ð ï ð ï ð ï ð ï ð ï ð ï ð ï

Maxim Yu. Khlopov
VIA, APC Laboratory, Paris, France and National Research Nuclear University "Moscow Engineering and Physics Institute" Centre for Cosmoparticle physics "Cosmion", Moscow, Russia

- COSMOPARTICLE physics ­ fundamental relationship of COSMOlogy and PARTICLE physics
«-100», 100- .. 20 , 2014, ,


Outlines
· Cosmological impact of new stable particles: direct and indirect searches for dark matter · Cosmological patterns of particle symmetry breaking: archioles, massive PBH clusters, antimatter domains .


The bedrocks of modern cosmology
Our current understanding of structure and evolution of the Universe implies three necessary elements of Big Bang cosmology that can not find physical grounds in the standard model of electroweak and strong interactions. They are:

· Inflation · Baryosynthesis · Dark matter/energy
All these phenomena imply extension of the Standard Model of Strong (QCD) and Electroweak Interactions. On the other hand, studies of physics Beyond the Standard Model involve Cosmology for their probe.
3


COSMOPARTICLE PHYSICS studies the fundamental relationship of COSMOlogy and PARTICLE PHYSICS in the complex cross-disciplinary physical and astronomical research


THE PUZZLES OF DARK MATTER SEARCH


Composition of the Universe
cr
b 0.044
DM



CMB

0.5 10

-4

0.20 1.0

0.7
tot

Baryonic matter consists of atoms

Can dark Matter consist of Dark atoms?

6


Cosmological Dark Matter


DM

baryons

T T t

Cosmological Dark Matter explains: · virial paradox in galaxy clusters, · rotation curves of galaxies · dark halos of galaxies · effects of macro-lensing But first of all it provides formation of galaxies from small density fluctuations, corresponding to the observed fluctuations of CMB

To fulfil these duties Dark Matter should interact sufficiently weakly with baryonic matter and radiation and it should be sufficiently stable on cosmological timescale


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 conservation law should correspond to a (nearly) strict symmetry of microworld.


Dark matter and the mass of neutrino

In 1980 the experimental claims on the existence of the mass of electron neutrino about 30 eV lead to immediate cosmological consequence of the neutrino dominated Universe, In which massive neutrinos play the role of dark matter.


Direct seaches for Dark Matter


Direct search for DM (WIMPs)
DAMA/NaI (7 years) + DAMA/LIBRA (6 years)
total exposure: 1.17 tonâyr

R (t ) = S 0 + S m cos[ (t - t

0

)]

Confidence level 8.9

R.Bernabei et al, arXiv: 1007.0595, 4 July 2010

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

DAMA(NaI) under variety of assumptions

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

12


Direct Detection Nov. 2013
PDG update 2013 (1204.2373)

LHC: theory region has moved down and right
in a very specific way

Smoking gun of SUSY?
preLHC!

Confusion region gone

motivated by theory (SUSY)
L. Roszkowski, APC, 14/3/2014 MasterCode,

BayesFITS

13


Indirect searches for Dark Matter


Cosmic positron excess from DM?

Probably such indirect effect is detected in the cosmic positron fluxes. [figure from K.M.Belotsky et al. arXiv:1403.1212]


DARK MATTER FROM CHARGED PARTICLES?


Baryonic Matter ­ atoms of stable quarks and charged lepton (electron)
· Ordinary matter consists of atoms · Atoms consist of nuclei and electrons. · Electrons are lightest charged particles ­ their stability is protected by the conservation of electric charge. · Nuclei consist of nucleons, whose stability reflects baryon charge conservation.

In ordinary matter stable elementary particles are electrically charged, but bound in neutral atoms.


Dark Matter from Charged Particles?
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

M =m
· ·

Pl

m Pl m

2

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.


« No go theorem » for -1 charge components
· If composite dark matter particles are « atoms », binding positive P

and negative E charges, all the free primordial negative charges E bind with He-4, as soon as helium is created in SBBN.

· Particles E with electric charge -1 form +1 ion [E He]. · This 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 particles E

have electric charge -2.


Nuclear-interacting composite dark matter: O-helium « atoms »
If we have a stable double charged particle X -- in excess over its partner X++ it may create Helium like neutral atom (O-helium) at temperature T > Io
Where:
4

2 2 I o = Z He Z 2 m

He

= 1.6 MeV

This means that it would rapidly create a neutral atom, in which all X -- are bound

He is formed at T ~100 keV (t~100 s)

X--+4He => (X He) +
The Bohr orbit of O-helium « atom » is of the order of radius of helium nucleus.

Ro = 1/ ( ZZ He m
References
1. M.Yu. Khlopov, JETP Lett. 83 (2006) 1;

He

)

= 2 10

-13

cm

2. D. Fargion, M.Khlopov, C.Stephan, Class. Quantum Grav. 23 (2006) 7305; 2. M. Y. Khlopov and C. Kouvaris, Phys. Rev. D 77 (2008) 065002]

20


Constituents of composite dark matter
Few possible candidates for -2 charges:
Stable doubly charged "leptons" with mass >100 GeV (~1 TeV range):

·AC « leptons » from almost commutative geometry
D. Fargion, M.Khlopov, C.Stephan, Class. Quantum Grav. 23 (206) 7305

· Technibaryons and technileptons from Walking Technicolor (WTC)
M. Y. Khlopov and C. Kouvaris, Phys. Rev. D 77 (2008) 065002; M. Y. Khlopov and C. Kouvaris, Phys. Rev. D 78 (2008) 065040

Hadron-like bound states of:

·Stable U-quark of 4-th family in Heterotic string phenomenology
M.Yu. Khlopov, JETP Lett. 83 (2006) 1

·Stable U-quarks of 5th family in the approach, unifying spins and

charges

N.S. Mankoc Borstnik, Mod. Phys. Lett. A 10 (1995) 587 M.Yu.Khlopov, A.G.Mayorov, E.Yu.Soldatov (2010), arXiv:1003.1144 21


O-HELIUM DARK MATTER


O-helium dark matter
T < Tod = 1keV
TRM = 1eV
M
od

·

nb v ( mp m ) t <1 o
mPl TRM = 109 M = mPl T Tod od
2

· ·
Sun

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


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


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.


O-HELIUM DARK MATTER IN UNDERGROUND DETECTORS


O-helium concentration in Earth
The 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


Annual modulation of O-helium concentration in Earth
The equilibrium concentration, which is established in the matter of underground detectors, is given by

where is given by

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

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.


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 · 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

OHe + ( A, Z ) [OHe( A, Z )] + is possible, in which only a few keV energy is released. Other inelastic processes are suppressed


Potential of OHe-nucleus interaction
r r r

UXnuc= -2Z 1 + 1 exp-2r ro r r ( o

)

U

Stark

2 Z 9 3 =- 4 ro r2

UCoul

2Z 2Z =+ - r

(Z +2) Uosc = - R

1-

r R



2




V

Formation of OHe-nucleus bound system shielded Coulomb Due to
VCoul
potential of X, Stark effect and tail of nuclear Yukawa force OHe attracts the nucleus. Nuclear attarction causes OHe excitation and Coulomb repulsion is switched on. If the system emits a photon, OHe forms a bound state with nucleus but beyond the nucleus with binding energy of few keV.

X

--
1 3

He

RA A

R

A

RA + ro + r

A

r

E~few keV

VStark + Vshield + Vnuc

Vosc


Few keV Level in OHe-nucleus system
· The problem is reduced to a quantum mechanical problem of energy level of OHe-nucleus bound state in the potential well, formed by shielded Coulomb, Stark effect and Yukawa tail attraction and dipole-like Coulomb barrier for the nucleus in vicinity of OHe. The internal well is determined by oscillatory potential of X in compound (Z+2) nucleus, in which He is aggregated. · The numerical solution for this problem is simplified for rectangular wells and walls, giving a few keV level for Na.


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)


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 system in DAMA experiment should not exceed 6 keV, being in the range 2-4 keV.


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

This value should be compared with the integrated over energy bins signals in DAMA/NaI and DAMA/LIBRA experiments and the results of these experiments can be reproduced for

ENa = 3keV


Excessive positrons in Integral
Taking 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.


Excessive positrons in Integral from dark atoms­ high sensitivity to DM distribution

J.-R. Cudell, M.Yu.Khlopov and Q.Wallemacq Dark atoms and the positron-annihilation-line excess in the galactic bulge. Advances in High Energy Physics, vol. 2014, Article ID 869425, : arXiv: 1401.5228


A solution for cosmic positron excess?
· In WTC: if both technibaryons UU and technileptons are present, CDMS, LUX results constrain WIMP-like (UU ) component to contribute no more than 0,0001% of total DM density. · Decays of positively charged UU->l+ l + 21 with a lifetime of about 10 s and mass 700-1000 GeV can explain the excess of cosmic positrons, observed by PAMELA and AMS02


Cosmic positron excess from double charged constituents of dark atoms

[K.M.Belotsky et al. arXiv:1403.1212]


PRIMORDIAL NONLINEAR STRUCTURES


Strong nonhomogeneities in nearly homogeneous and isotropic Universe
· The standard approach is to consider homogeneous and isotropic world and to explain development of nonhomogeneous structures by gravitational instability, arising from small initial fluctuations.
<< 1

<< 1

·

However, if there is a tiny component, giving small contribution to total density,

i <<

its strong nonhomogeneity

i (

)i

>1

= ( i +

is compatible with small nonhomogeneity of the total density

)

(

i



i

)( i )

<< 1

Such components naturally arise as consequences of particle theory, sheding new light on galaxy formation and reflecting in cosmic structures the fundamental structure of microworld.


Cosmological Reflections of Microworld Structure
· Dark Matter should be present in the modern Universe, and thus be stable on cosmological scale. This stability reflects some Conservation Law, which prohibits DM decay. Following Noether's theorem this Conservation Law should correspond to a (nearly) strict symmetry of microworld. Indeed, all the particles - candidates for DM reflect the extension of particle symmetry beyond the Standard Model. · In the early Universe at high temperature particle symmetry was restored. Transition to phase of broken symmetry in the course of expansion is the source of topological defects (monopoles, strings, walls...).


Cosmological Phase transitions 1.
· At high temperature T > T cr spontaneously broken symmetry is restored, owing to thermal corrections to Higgs potential
m2 2 4 V ( , T = 0) = - + V ( , T ) 2 4 · When temperature falls down m T = T cr = m2 2 + = CT 2 - 2 4 below
4

transition to phase with broken symmetry takes place.


Cosmological Phase transitions 2.
· Spontaneously broken symmetry can be restored on chaotic inflationary stage, owing to corrections in Higgs potential due to interaction of Higgs field with inflaton 2 m2 2 4 m2 2 4 + + V ( , ) = - V ( , = 0 ) = - 2 4 2 4 · When inflaton field rolls down below m = cr transition to phase with broken symmetry takes place.


Topological defects
· In cosmological phase transition false (symmetric) vacuum goes to true vacuum with broken symmetry. Degeneracy of true vacuum states results in formation of topological defects. · Discrete symmetry of true vacuum = ± f leads to domains of true vacuum with +f and -f and false vacuum wall on the border. [Zeldovich, Kobzarev, Okun, 1975] · Continuous degeneracy = f exp(i ) results in succession of singular points surrounded by closed paths with = 2 . Geometrical place of these points is line ­ cosmic string. · SU(2) degeneracy results in isolated singular points ­ in GUTs they have properties of magnetic monopoles.


Strong Primordial nonhomogeneities from the early Universe
· Cosmological phase transitions in inflationary Universe can give rise to unstable cosmological defects, retaining a replica in the form of primordial nonlinear structures (massive PBH clusters, archioles). · Nonhomogenous baryosynthesis (including spontaneous baryosynthesis and leptogensis) in its extreme form can lead to antimatter domains in baryon asymmetrical inflationary Universe. Strong nonhomogeneities of total density and baryon density are severely constrained by CMB data at large scales (and by the observed gamma ray background in the case of antimatter). However, their existence at smaller scales is possible.


U(1) model
V ( ) =


2

(
f

2

-f

2

)

After spontaneous symmetry breaking infinitely degenerated vacuum

= fei

experiences second phase transition due to the presence (or generation by instanton effects)

V ( ) = 4 (1- cos( f
to vacuum states

))

f = 0,2 ,...
In particular, this succession of phase transitions takes place in axion models


Axion


Topological defects
·



Spontaneous breaking of U(1) symmetry results in the continuous degeneracy of vacua. In the early Universe the transition to phase with broken symmetry leads to formation of cosmic string network.

·

The tilt in potential breaks continuous degeneracy of vacua. In the result string network converts into wallsbounded-by-strings structure in the second phase transition.


Unstable topological defects
· The first phase transition gives rise to cosmic string network. · This network converts in the second phase transition into walls-bounded-by-strings structure (walls are formed between strings along the surfaces = ), which is unstable. · However, the energy density distribution of coherent oscillations of the field follows the walls-bounded-by-strings structure.


Archioles structure
· Numerical studies revealed [Vachaspati,Vilenkin, 1984] that ~80% of string length corresponds to infinite Brownian lines, while the remaining ~20% of this length corresponds to closed loops with large size loops being strongly suppressed. It corresponds to the well known scale free distribution of cosmic strings. The fact that the energy density of coherent oscillations reflects this property is much less known. It leads to a large scale correlation in this distribution, called archioles [Khlopov,Sakharov, 1994; Khlopov, Sakharov, Sokoloff, 1996; 1999] Archioles offer possible seeds for large scale structure formation.

·

·


Massive Primordial Black Holes
· Any object can form Black hole, if contracted within its gravitational radius. It naturally happens in the result of evolution of massive stars (possibly, star clusters). · In the early Universe Black hole can be formed, if within cosmological horizon expansion can stop [Zeldovich, Novikov, 1966]. Since in the early Universe the total mass within horizon is small, it seems natural to expect that such Primordial Black holes should have very small mass (much smaller, than the mass of stars). · However, cosmological consequences of particle theory can lead to mechanisms of intermediate and even supermassive BH formation.


Closed walls formation in Inflationary Universe

If the first U(1) phase transition takes place on inflationary stage, the value of phase , corresponding to e-folding N~60, fluctuates

H

infl

(2f )


Such fluctuations can cross

and after coherent oscillations begin,regions with > occupying relatively small fraction of total volume are surrounded by massive walls


Massive PBH clusters
Each massive closed wall is accompanied by a set of smaller walls. As soon as wall enters horizon, it contracts and collapses in BH. Each locally most massive BH is accompanied by a cloud of less massive BHs. The structure of such massive PBH clouds can play the role of seeds for galaxies and their large scale distribution.


Spectrum of Massive BHs
· The minimal mass of BHs is given by the condition that its gravitational radius exceeds the width of d 2 f 2 wall ( ) 2 2M 2f mPl rg = 2 > d = 2 Mmin = f mPl · The maximal mass is given by the condition that pieces of wall do not dominate within horizon, before the whole wall enters the horizon
R< 3

tot

w

M

max

mPl mPl Mmax = f f M min

2

2

mPl = f

2


GW signals from closed wall collapse and BHs merging in clouds
· Closed wall collapse leads to primordial GW spectrum, 0 = 31011( f )Hz peaked at with energy density up to

GW 10 ( f mPl
-4

)

· At , GW · For 1 < < 10 8 GeV 310-3 Hz < 0 < 3105 Hz
f ~ 10 14 GeV



~ 10 .-

9

· Merging of BHs in BH cluster leads to signals accesible to LISA test.


Nonhomogeneous spontaneous baryosynthesis
Model of spontaneous baryosynthesis

naturally leads to nonhomogeneity of baryon excess and to generation of antibaryon excess in some regions

Sufficiently large domains of antimatter survive to the present time


Survival of antimatter domains
Diffusion of baryons and antibaryons to the border of domain results in eating of antimatter by surrounding baryonic matter. where

The minimal surviving scale is given by

which is about


Antimatter in galaxies
Numerical simulations show that within the modern horizon possible amount of antimatter domains, with the size exceeding the survival scale and thus surviving to the present time, can be comparable with the total number of galaxies. In our Galaxy from 1000 to 100000 antimatter stars can exist in a form of antimatter globular cluster (Khlopov, 1998). Being in halo, such cluster is a faint gamma ray source, but antimatter from it pollutes Galaxy and can be observed indirectly by annihilation, or directly as anti-meteorites or antinuclei in cosmic rays.


Cosmic antihelium test for antimatter stars in Galaxy

·

·

· ·

Nonhomogeneous baryosynthesis in extreme form leads to antimatter domains in baryon asymmetrical Universe To survive in the surrounding matter domain should be sufficiently large, and to have sufficiently high internal antibaryon density to form stars. It gives minimal estimation of possible amount of antimatter stars in Galaxy The upper limit comes from observed gamma background Assuming that antihelium component of cosmic rays is proportional to the fraction of antimatter stars in the total mass of Galaxy, it is possible to test this hypothesis in AMS-02 experiment


Conclusion
The puzzle of our origin and existence still retains in the multiverse of cosmological scenarios and particle physical models underlying them. Zeldovich's dream on the complete cosmological model based on the true particle theory remains the challenge of cosmoparticle physics.


Basic ideas of cosmoparticle physics in studies of New Physics, underlying Modern Cosmology
· · · Physics beyond the Standard model can be studied in combination of indirect physical, astrophysical and cosmological effects New symmetries imply new conserved charges. Strictly conserved charge implies stability of the lightest particle, possessing it. New stable particles should be present in the Universe. Breaking of new symmetries implies cosmological phase transitions. Cosmological and astrophysical constraints are supplementary to direct experimental search and probe the fundamental structure of particle theory Combination of physical, cosmological and astrophysical effects provide an overdetermined system of equations for parameters of particle theory

·

COSMOlogy
Physical scale

PARTICLE PHYSICS New physics

Extremes of physical knowledge converge in the mystical Uhrohboros wrong circle of problems, which can be resolved by methods of Cosmoparticle physics


International Virtual Institute of Astroparticle Physics (CosmoVIA)
A possible regular interactive form of collaboration in crossdisciplinary study of fundamental relationship between micro- and macro-worlds


Possible submissions
· WSPC Book Project « Indirect Effects of Dark Matter Physics (12193) » (~30pp) · Special issue of the MPLA "Dark Matter Particle Candidates" (~10pp)
You are invited to contribute these issues before the end of 2014. Please send your submissions to khlopov@apc.univ-paris7.fr