Bled Workshops in Physics Vol. 19, No. 2 A Proceedings to the 21 st Workshop What Comes Beyond ... (p. 314) Bled, Slovenia, June 23-July 1, 2018 15 Beyond the Standard Models of Particle Physics and Cosmology M.Yu. Khlopov * Institute of Physics, Southern Federal University Stachki 194, Rostov on Don 344090, Russia Abstract. The modern Standard cosmological model of inflationary Unvierse and baryosyn-thesis deeply involves particle theory beyond the Standard model (BSM). Inevitably, models of BSM physics lead to cosmological scenarios beyond the Standard cosmological paradigm. Scenarios of dark atom cosmology in the context of puzzles of direct and indirect dark matter searches, of clusters of massive primordial black holes as the source of gravitational wave signals and of antimatter globular cluster as the source of cosmic antihelium are discussed. Povzetek. V standardni kozmoloski model inflacijskega vesolja in tvorbe barionov vključi avtor tudi teorijo osnovnih delcev in polj, kar razsiri standardni model. Avtor obravnava model "temnih atomov", to je atomov, ki vsebujejo fermione družine z veliko maso. Predstavi prispevek temnih atomov v experimentih, ki naj bi detektirali temno snov, vlogo temnih atomov kopic masivnih prvotnih crnih lukenj, ki sevajo gravitacijske valove ter v globularnih kopicah antisnovi, ki naj bi bil izvor antihelija v vesolju. Keywords: cosmoparticle physics, inflation, baryosynthesis, dark matter, dark atoms, clusters of massive primordial black holes, antimatter, double charged particles, nuclear reactions, nucleosynthesis PACS: 12.60.-i; 95.35.+d; 14.80.-j; 21.90.+f; 36.10.-k; 98.80.-k; 98.80.Cq; 98.80.Ft; 04.70.-s; 15.1 Introduction The basis of the modern Standard cosmological paradigm, involving inflation, baryosynthesis and dark matter as its neccessary basic elements, is related to new physics predicted in theory beyond the Standard model (BSM) of elementary particles (see e.g. Ref. [1] for review and reference). However, BSM models, reproducing the necessary basic elements of the modern cosmology, inevitably contain additional model dependent consequences that lead beyond the Standard cosmological scenario [2]. Methods of cosmoparticle physics, studying fundamental relationship of cosmology and particle physics in the combination of its physical, astrophysical and * E-mail: khlopov@apc.in2p3.fr 15 Beyond the Standard Models of Particle Physics and Cosmology 315 cosmological signatures, involve such model dependent cosmological predictions to probe models of BSM physics and cosmological scenarios, based on them. [3-5]. Here we show that BSM physics leads to cosmological scenarios accomplished by nontrivial deviations from the Standard cosmological model that deserve special interest in the context of the recent experimental progress. We address a possibility of existence of stable double charged particles O bound with primordial helium in neutral nuclear interacting O-helium dark atoms (Section 15.2) and consider advantages of this scenario to resolve puzzles of direct and indirect dark matter searches, as well as the open problems of OHe interaction with matter. We show that BSM physics of inflationary models that naturally leads to strong primordial inhomogeneities and to clusters of massive primordial black holes, in particular, is possibly reflected in the gravitational wave signal from massive black hole coalescence (Section 15.3). We discuss in Section 15.4 existence of antimatter stars in our Galaxy, originated from nonhomogeneous baryosynthe-sis in baryon asymmetrical Universe and reflected in cosmic antihelium fluxes, possibly detected by AMS02 [6,7]. 15.2 Dark atom physics and cosmology In the simplest case physics of dark matter is reduced to prediction by BSM model of new neutral elementary weakly interacting massive particle (WIMP). This type of prediction is beyond the standard model of elementary particles, but fits perfectly well the standard cosmological LambdaCDM paradigm. Super-symmetric (SUSY) models, predicting WIMP candidates, seemed to support this simple approach to dark matter physics. However negative results of experimental underground WIMP searches, as well as of collider searches for SUSY particles appeal to other possible BSM solutions for the dark matter problem. Possibly, SUSY physics and cosmology corresponds to superhigh energy scales as discussed in this Volume in [8]. In fact, the necessary conditions for dark matter candidates to be stable, satisfy the measured dark matter density and be decoupled from plasma and radiation at least before the beginning of matter dominated stage in no case demand these particle candidates to be weakly or superweakly interacting. Even nuclear interacting particles can play the same role due to decoupling of the gas of such particles from plasma and radiation before the end of radiation dominated stage. It gives rise to models of dark matter in the form of Strongly Interacting Massive Particles (SIMPs) [9-14]. By definition dark matter should be 'dark', nonluminous, what seem to favor neutral elementary particles. However ordinary atomic matter is neutral but it is composite and consists of electriclly charged particles (nuclei and electrons). In the same way O-helium dark atoms represent a specific example of composite SIMPs, in which hypothetical double charged O particles are bound with primordial helium nuclei by ordinary Coulomb force [15-20]. 316 M.Yu. Khlopov 15.2.1 OHe and O-nuclearites The main problem for hypothetical stable charged particles is their absence in the matter. If they do exist, they should be bound with ordinary matter and form anomalous isotopes. Severe experimental constraints on such isotopes, on anomalous hydrogen especially, seem to exclude a possibility for stable charged particles. However, if there exist stable particles with charge -2 in excess over corresponding particles with charge +2, such negatively charged particles are captured by primordial helium and form neutral OHe dark atom. There are various models, in which such stable -2 charged particles O are predicted [15-20]. Moreover, if these particles possess electroweak SU(2) gauge charges, their excess can be equilibrated by electroweak sphaleron transitions with baryon excess, as it is the case in Walking Technicolor models [17]. The general analysis of the bound states of single O with nuclei was developed in a simple model [21-23]. For small nuclei the Coulomb binding energy is like in hydrogen atom and is given by Eb = lz2ZOa2Amp. (15.1) For large nuclei O is inside nuclear radius and the harmonic oscillator approximation is valid for the estimation of the binding energy Eb — 3 ( ZZ°a _ 1 ( ZZOa )1/2). lb = 2_ R(AmpRJ ' J. (15.2) Here Z is the charge of nucleus, A is its atomic number, R is radius of nucleus, ZO = 2 is the charge of O , mp is the proton mass and a = 1/137 is the fine structure constant. In the case of OHe ZZO aAmp R < 1, what proves its Bohr-atom-like structure (see [19,20] for review and references). However, the radius of Bohr orbit in these "atoms" [15,17] ro ~ 1/(ZOZHeamHe) ~ 2 • 10-13 cm is of the order the size of He nucleus. Therefore the corresponding correction to the binding energy due to non-point-like charge distribution in He nucleus is significant. O particles are either elementary lepton-like states, or clusters of heavy U quarks with charge -2/3 UUU, which have strongly suppressed QCD interaction. In the contrary to ordinary atoms OHe has heavy lepton-like core and nuclear interacting shell. If multiple O are captured by a heavy nucleus, the corresponding neutral bound system can acquire the form of O-nuclearites, in which negative charge of O is compensated by posistive charge of protons in the nucleus [24]. The energy of such a O-nuclearite is given by [24] £ — _16MeV- A d3r(np _ 2no)V d3r ^+. (153) Here the first term is the volume energy of the atomic nucleus with atomic number A, next two terms describe the electromagnetic energy, and fO — d3r Pf,q 2 2 " (15.4) n2 2mO 15 Beyond the Standard Models of Particle Physics and Cosmology 317 is the kinetic energy of the O-fermions of the mass mO; V = —e^ is the potential well for the electron in the field of the positive charge (e > 0, ^ > 0) and on the other hand it is the potential well also for the protons in the field of the negative charge of O-particles. The most energetically favorable O-particle distribution inside the nucleus is that follows the proton one, fully compensating the Coulomb field. Thereby O-particles, if their number were NO > A/4, would be re-distributed to minimize the energy, and finally the density of O inside the atomic nucleus becomes nO = np/2 = (n0/2) 0(r — R) for O-nuclearite, that corresponds to V = const for r < R. Excessive O-particles are pushed out. 15.2.2 Cosmoparticle physics of OHe model After the Standard Big Bang Nucleosynthesis (SBBN) O charged particles capture 4He nuclei in neutral OHe "atoms" [15]. For the mass of O mO ~ 1 TeV, O abundance is much smaller than helium abundamce, so that He is in excess in such capture, making the abundance of frozen out free O exponentially small. The cosmological scenario of OHe Universe involves only one parameter of new physics — the mass of O . Such a scenario is insensitive to the properties of O (except for its mass), since the main features of the OHe dark atoms are determined by their nuclear interacting helium shell. Before the end of radiation domination stage the rate of expansion exceeds the rate of energy and momentum transfer from plasma to OHe gas and the latter decouples from plasma and radiation. Then OHe starts to dominate at the Matter Dominated stage, playing the role of Warmer than Cold Dark Matter in the process of Large Scale Structure formation[15,19]. This feature is due to conversion of small scale fluctuations in acoustic waves before OHe decoupling and to their corresponding suppression. However, the suppression of such fluctuations is not as strong as the free streaming suppression for few keV dark matter particles in Warm Dark matter models. In terrestrial matter OHe dark atoms are slowed down and cannot cause significant nuclear recoil in the underground detectors, making them elusive for detection based on nuclear recoil. The positive results of DAMA experiments (see [25] for review and references) can find in this scenario a nontrivial explanation due to a low energy radiative capture of OHe by intermediate mass nuclei [19,1,20]. This explains the negative results of the XENON100 and LUX experiments. The rate of this capture is proportional to the temperature: this leads to a suppression of this effect in cryogenic detectors, such as CDMS. OHe collisions in the central part of the Galaxy lead to OHe excitations, and de-excitations with pair production in E0 transitions can explain the excess of the positron-annihilation line, observed by INTEGRAL in the galactic bulge [1,20,26,27]. Due to the large uncertainty of DM distribution in the galactic bulge this interpretation of the INTEGRAL data is possible in a wide range of masses of O-helium with the minimal required central density of O-helium dark matter at mO = 1.25 TeV. For smaller or larger values of mo one needs larger central density to provide effective excitation of O-helium in collisions. Current analysis 318 M.Yu. Khlopov favors lowest values of central dark matter density, making possible O-helium explanation for this excess only for a narrow window around this minimal value. In a two-component dark atom model, based on Walking Technicolor, a sparse WIMP-like component of atom-like state, made of positive and negative doubly charged techniparticles, is present together with the dominant OHe dark atoms. Decays of doubly positive charged techniparticles to pairs of same-sign leptons can explain [28] the excess of high-energy cosmic-ray positrons, found in PAMELA and AMS02 experiments[29-32]. Since even pure lepton decay channels are inevitably accompanied by gamma radiation the important constraint on this model follows from the measurement of cosmic gamma ray background in FERMI/LAT experiment[33]. The multi-parameter analysis of decaying dark atom constituent model determines the maximal model independent value of the mass of decaying +2 charge particle, at which this explanation is possible mO < 1TeV. One should take into account that even in this range hypothesis on decaying composite dark matter, distributed in the galactic halo, can lead according to [34] to gamma ray flux exceeding the measurement by FERMI/LAT. It can make more attractive interpretation of these data by an astrophysical pulsar local source[35] or by some local source of dark matter annihilation or decay. Experimental probes for OHe dark matter at the LHC strongly differ from the usual way of search for dark matter at acelerators, involving missed energy and momentum detection. Pending on the nature of the double charge constituents it may be search for new stable U-hadrons (heavy stable hadrons that appear in the result of production of UU pair) or search for stable double charged lepton-like particles. In the first case there are applicable constraints from the search for supersymmetric R-hadrons, having similar experimental signatures and giving the minimal mass for UUU close to 3 TeV. It excludes OHe interpretation of the cosmic positron anomalies in terms of heavy quark cluster constituents of OHe. The possibility to interpret cosmic positron anomalies in terms of OHe cos-tituents that appear in the experiments as stable lepton-like double charged particles is also close to complete test. The ATLAS and CMS collaborations at the LHC are searching for the double charged particles since 2011 [36-38]. The most stringent results achieved so far exclude the existence of such particles up to their mass of 680 GeV. This value was obtained by both ATLAS and CMS collaborations independently. It is expected that if these two collaborations combine their independently gathered statistics of LHC Run 2 (2015-2018), the lower mass limit of double charged particles could reach the level of about 1.3 TeV. It will make search for exotic long-living double charged particles an experimentum crucis for interpretation of low and high energy positron anomalies by composite dark matter [39,40]. The successful and self-consistent OHe scenario implies the existence of dipole Coulomb barrier, arising in OHe-nuclear interaction and supporting dominance of elastic OHe-nuclear scattering. This problem of nuclear physics of OHe remains the main open question of composite dark matter, which implies correct quantum mechanical solution [41]. The lack of such a barrier and essential contribution 15 Beyond the Standard Models of Particle Physics and Cosmology 319 of inelastic OHe-nucleus processes seem to lead to inevitable overproduction of anomalous isotopes [42]. The advantages of the qualitative picture of OHe scenario appeal to increase the efforts to solve this problem. 15.3 Primordial massive black hole clusters The standard cosmological model considers homogeneous and isotropic Universe as the result of inflation. The observed celestial objects and strong inhomogeneities are evolved from small primordial density fluctuations that are also originated from small fluctuations of the inflaton field. It seems that there is no room for strong primordial inhomogeneities in this picture. Moreover, the existence of large scale inhomogeneities at the scales ^ 100Mpc is excluded by the measured isotropy of CMB. However, BSM physics, predicting new fields and mechanisms of symmetry breaking, adds new elements in this simple scenario that provide the existence of strong primordial inhomogeneities. Such predictions are compatible with the observed global homogeneity and isotropy of the Universe, if the strongly inho-mogeneous component i with (6p/p]i ~ 1 contributes into the total density ptot whithin the observed level of the large scale density fluctuations (Sp/p) = S0 C 1. It implies either large scale inhomogeneities, suppressed by the small contribution of the component i into the total density pi/ptot < S0, or inhomogeneities at small scales. A simple example of an axion-like model with U(1) symmetry broken spontaneously and then explicitly illustrates these two possible forms of strong primordial inhomogeneities. In this model spontaneous U(1) symmetry breaking is induced by the vacuum expectation value If the first phase transion takes place after inflation at T = f and f ^ A, the potential Eq. (15.7) doesn't influence continuous degeneracy of vacua on 9 and string network is formed, which is converted in a walls-surrounded-by-strings network, separating regions with discrete vacuum degeneracy 9vac + 0,2n,... after the second phase transition at T = A. The vacuum structure network is unstable and decays, but the energy density distribution of 9 field oscillations is strongly inhomogeneous and retains the large scale structure of this network, as it was shown in the example of axion models in [43-45]. To fit the observational constraints on the inhomogeneity at large scales the contribution into the total density of such structure, called archioles, should be suppressed. It causes serious (15.5) (15.6) (15.7) 320 M.Yu. Khlopov problem for CDM models, in which the dominant form of dark matter is explained by axions [43-45]. If the first phase transition takes place at the inflational stage and f ^ A, as it was considered in [46], there appears a valley relative to values of phase in the field potential in this period. Fluctuations of the phase 0 along this valley, being of the order of A0 ~ H/(2nf) (here H is the Hubble parameter at inflational stage) change in the course of inflation its initial value within the regions of smaller size. Owing to such fluctuations, for the fixed value of 06o in the period of inflation with e-folding N = 60 corresponding to the part of the Universe within the modern cosmological horizon, strong deviations from this value appear at smaller scales, corresponding to later periods of inflation with N < 60. If 06o < n, the fluctuations can move the value of 0N to 0N > n in some regions of the Universe. After reheating, when the Universe cools down to temperature T = A the phase transition to the true vacuum states, corresponding to the minima of Veb takes place. For 0N < n the minimum of Veb is reached at 0vac = 0, whereas in the regions with 0N > n the true vacuum state corresponds to 0vac = 2n. For 06o < n in the bulk of the volume within the modern cosmological horizon 0vac = 0. However, within this volume there appear regions with 0vac = 2n. These regions are surrounded by massive domain walls, formed at the border between the two vacua. Since regions with 0vac = 2n are confined, the domain walls are closed. After their size equals the horizon, closed walls can collapse into black holes. The mass range of formed BHs is constrained by fundamental parameters of the model f and A. The maximal BH mass is determined by the condition that the wall does not dominate locally before it enters the cosmological horizon. Otherwise, local wall dominance leads to a superluminal a