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SUMMARY:Stabilization of the extra dimension size in RS model by bulk Higg
 s field
DTSTART;VALUE=DATE-TIME:20161011T143000Z
DTEND;VALUE=DATE-TIME:20161011T144500Z
DTSTAMP;VALUE=DATE-TIME:20260814T154822Z
UID:indico-contribution-100-773@cern.ch
DESCRIPTION:Speakers: Vadim Egorov (M.V.Lomonosov Moscow State University\
 , Skobeltsyn Institute of Nuclear Physics (SINP MSU))\nAn extension of the
  Standard Model is considered\, which is built on the basis of the Randall
 -Sundrum model with two branes. The metric of the background solution is n
 ot flat\, which allows to solve the hierarchy problem of the gravitational
  interaction. In the case of unstabilized interbrane distance the model pr
 edicts the existence of the "strongly" coupled massless scalar mode\, the 
 radion\, which contradicts the experimental data. In the present work the 
 stabilization of the extra dimension size is achieved with the help of the
  five-dimensional Higgs field\, which plays the role of the Goldberger-Wis
 e filed. The stabilization makes the radion massive\, and all the fermion 
 fields\, which are assumed to be localized on the TeV brane\, get their ma
 sses due to the interaction with the boundary value of the Higgs field. Th
 e gauge invariance of the theory demands that the electroweak gauge fields
  also live in the bulk. The equations of motion for the background field c
 onfigurations are obtained\, the second variation Lagrangian for the field
  fluctuations against a background solution is derived and the equations o
 f motion for them are obtained. The interactions of the bulk Higgs field w
 ith the multidimensional gauge and fermion fields are studied and possible
  values of the model parameters are estimated.\n\nhttps://indico.particle.
 mephi.ru/event/4/contributions/773/
LOCATION:Milan Hotel Rossini
URL:https://indico.particle.mephi.ru/event/4/contributions/773/
END:VEVENT
BEGIN:VEVENT
SUMMARY:The AEgIS experiment at CERN
DTSTART;VALUE=DATE-TIME:20161011T131500Z
DTEND;VALUE=DATE-TIME:20161011T133000Z
DTSTAMP;VALUE=DATE-TIME:20260814T154822Z
UID:indico-contribution-100-759@cern.ch
DESCRIPTION:Speakers: Germano Bonomi (University of Brescia and INFN PAVIA
 )\nThe main goal of the AEgIS collaboration is the measurement of the grav
 itational acceleration of antimatter in the Earth field. The AEgIS experim
 ent is presently taking data at the CERN Antiproton Decelerator (AD) facil
 ity. The first step of the measurement is the creation of a beam of anti-h
 ydrogen through the combination of antiprotons and positrons. The beam wil
 l be directed toward a moiré deflectometer able to detect the vertical di
 splacement due to the interaction of the neutral anti-atoms with the Earth
  gravitational field. This measurement would be of great interest as it wo
 uld probe the Weak Equivalence Principle of General Relativity with antima
 tter. \nThe experimental apparatus\, the measurement strategy and techniqu
 e and the results obtained so far will be presented.\n\nhttps://indico.par
 ticle.mephi.ru/event/4/contributions/759/
LOCATION:Milan Hotel Rossini
URL:https://indico.particle.mephi.ru/event/4/contributions/759/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Application of  conventionality in distant simultaneity to integra
 l covariant formulation of conservation laws
DTSTART;VALUE=DATE-TIME:20161011T141500Z
DTEND;VALUE=DATE-TIME:20161011T143000Z
DTSTAMP;VALUE=DATE-TIME:20260814T154822Z
UID:indico-contribution-100-716@cern.ch
DESCRIPTION:Speakers: Valery Stepanov (Russian Federation)\nIn 1930\, Reic
 henbach established the possibility of generalization of Einstein's defini
 tion of synchronizing spatially separated a couple of hours\, introducing 
 Reichenbach parameter that varies from zero to one\, which defines one-way
  speed of light. A fundamental constant is the average speed of light back
  and forth. The independence of this observed value of the choice of inert
 ial reference systems supported by the Michelson-Morley experiment.Then Jo
 hn A Winnie in 1970\, formulated a generalization of the special theory of
  relativity to the case of generalized synchronization Reichenbach. Curren
 tly\, there is discussion about the consistency with the physical experime
 nts of Reichenbach's thesis of the conventionality of simultaneity spatial
 ly separated clocks.\n\nWithout entering into this discussion about the ph
 ysical reality according to Reichenbach's thesis in this paper\, we propos
 e the possibility of using non-standard synchronization in the relativisti
 c -invariant integral formulation of the laws of conservation of charge\, 
 the energy - momentum\, and other conserved quantities.\n\nFor two inertia
 l reference systems\, the relativity of simultaneity phonological paradigm
 atic events.Richard Feynman in his Nobel lecture gave an example of the de
 parture of electron-positron pair from the two ends of the rod of finite l
 ength. On the basis of the fact of the relativity of simultaneity of these
  two events\, he concluded that the local law of conservation of electric 
 charge for non-point objects.\n\nAt first\, for example\, in a textbook of
  Theoretical Physics Landau-Lifshitz theory of special relativity is formu
 lated in four-dimensional space-time of Minkowski. The equations of the dy
 namics of the material point is a relativistic generalization of Newton's 
 laws contain as a time parameter interval proportional to the proper time 
 of the moving material point\, which does not depend on clock synchronizat
 ion. By synchronizing the clocks do not depend on the energy\, momentum\, 
 and other conserved quantities.\n\nConsider the insular system of mutually
  motionless particles. The law of conservation of charge for this system i
 n differential form is expressed as the vanishing of the divergence of a f
 our-vector volumetric current density. To calculate the integral formulati
 on of the integral over the four-volume tube world lines of particles insu
 lar system\, forming a four-cylinder. This cylinder ends of two perpendicu
 lar to the world lines of the surfaces of simultaneous events belonging to
  the two points in time of the observer in his own frame of reference insu
 lar system. The lateral surface of the cylinder tends to spatial infinity\
 , where the charges are zero. In the four-dimensional Gauss theorem the vo
 lume integral is converted to the integral over a closed surface\, decayin
 g on the lateral surface and two bases. The result is an equality of two i
 ntegrals over the three-dimensional hypersurfaces for different points in 
 time. This means consistency\, i.e the conservation of the total charge in
 sular system. All the above corresponds to the integrated treatment of con
 servation laws in the course of Landau-Lifshitz. \n\nIf we move to the lab
 oratory reference system relative to which the insular system is moving in
 ertially\, then the hypersurface of simultaneity used in the insular syste
 m\, cease to be orthogonal to the temporal axis of the laboratory system. 
 \nBecause of the relativity of simultaneity there is an unequal one second
  parameter Reichenbach\, the speed of light is a fundamental constant is o
 nly an average. \nThe hypersurfaces of simultaneity in the four-dimensiona
 l Minkowski space are invariant geometric objects. In the area of the rela
 tivity of simultaneity\, you can choose any hypersurface\, while the numer
 ical values of the integrals of the remaining quantities do not depend on 
 the choice of hypersurfaces of simultaneity. Thus\, if you declare a custo
 m setting for the Reichenbach physically invalid\, it returns solemnly to 
 ensure the covariant integral formulation of the conservation laws of phys
 ical quantities.\n\nhttps://indico.particle.mephi.ru/event/4/contributions
 /716/
LOCATION:Milan Hotel Rossini
URL:https://indico.particle.mephi.ru/event/4/contributions/716/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Topological defects with power-law tails
DTSTART;VALUE=DATE-TIME:20161011T133000Z
DTEND;VALUE=DATE-TIME:20161011T134500Z
DTSTAMP;VALUE=DATE-TIME:20260814T154822Z
UID:indico-contribution-100-660@cern.ch
DESCRIPTION:Speakers: Roman Radomskiy (NRNU MEPhI)\nWe study scalar field 
 models with polynomial self-interaction. We write out conditions for the p
 otential which are to be satisfied for kinks with power-law asymptotics to
  exist. Using the model $\\varphi^8$ as an example\, we show that power-la
 w asymptotics of kinks lead to their long-range interaction. Within the co
 llective coordinate approximation we estimate the effective kink-antikink 
 potential and force in two cases: for kinks with power-law asymptotics\, a
 nd for kinks with exponential asymptotics. The numerical results from the 
 collective coordinate approximation are compared to asymptotic estimates o
 f the force of interaction via Manton's method. This long-range interactio
 n can have substantial consequences for phenomenology of physical systems\
 , the dynamics of which is described by field-theoretical models with poly
 nomial potentials. In particular\, domain walls in such models would inter
 act at large distances.\n\nhttps://indico.particle.mephi.ru/event/4/contri
 butions/660/
LOCATION:Milan Hotel Rossini
URL:https://indico.particle.mephi.ru/event/4/contributions/660/
END:VEVENT
BEGIN:VEVENT
SUMMARY:On black universes of multidimensional origin.
DTSTART;VALUE=DATE-TIME:20161011T130000Z
DTEND;VALUE=DATE-TIME:20161011T131500Z
DTSTAMP;VALUE=DATE-TIME:20260814T154822Z
UID:indico-contribution-100-640@cern.ch
DESCRIPTION:Speakers: Pavel Korolyov (PFUR\,)\nWe consider 6D manifolds wi
 th the structure M0 x M1 x  M2\, where M0 is 2D Lorentzian space-time whil
 e each of M1 and M2 can be a 2-sphere or a 2-torus.Among such geometries\,
  we find examples of regular solutions of 6D general relativity with a sca
 lar field as a source of gravity\, which depend on a single coordinate x r
 anging over the whole real axis\, with different asymptotic behavior at pl
 us and minus infinity. On one end\, it is a 4D de Sitter universe times sm
 all extra dimensions\, while on the other end there is some kind of a stat
 ic space-time. We thus obtain configurations called black universes\, look
 ing as a black hole on the static end and as an expanding universe on the 
 other\, and the cosmological expansion begins from a horizon.\n\nhttps://i
 ndico.particle.mephi.ru/event/4/contributions/640/
LOCATION:Milan Hotel Rossini
URL:https://indico.particle.mephi.ru/event/4/contributions/640/
END:VEVENT
BEGIN:VEVENT
SUMMARY:General properties and kinetics of spontaneous baryogenesis
DTSTART;VALUE=DATE-TIME:20161011T124500Z
DTEND;VALUE=DATE-TIME:20161011T130000Z
DTSTAMP;VALUE=DATE-TIME:20260814T154822Z
UID:indico-contribution-100-615@cern.ch
DESCRIPTION:https://indico.particle.mephi.ru/event/4/contributions/615/
LOCATION:Milan Hotel Rossini
URL:https://indico.particle.mephi.ru/event/4/contributions/615/
END:VEVENT
BEGIN:VEVENT
SUMMARY:On stability of exponential cosmological   solutions with non-stat
 ic volume factor in  the Einstein-Gauss-Bonnet  model
DTSTART;VALUE=DATE-TIME:20161011T134500Z
DTEND;VALUE=DATE-TIME:20161011T140000Z
DTSTAMP;VALUE=DATE-TIME:20260814T154822Z
UID:indico-contribution-100-591@cern.ch
DESCRIPTION:Speakers: Vladimir Ivashchuk (Center for Gravitation\, VNIIMS)
 \nA $(n+1)$-dimensional  gravitational model with Gauss-Bonnet term and co
 smological constant term  is  considered. When  ansatz with diagonal  cosm
 ological  metrics is adopted\,  the solutions  with  exponential dependenc
 e of scale factors:  $a_i \\sim \\exp{ ( v^i t) }$\, $i =1\, \\dots\, n $\
 , are considered.\n We study the stability of the solutions  with non-stat
 ic volume factor\, i.e. if\n $K(v) =  \\sum_{k = 1}^{n} v^k \\neq 0$.  We 
 prove that under certain restriction $R$ imposed  solutions with \n  $K(v)
  > 0$ are stable  while  solutions with $K(v)  0$ and  zero variation of t
 he effective gravitational constant  are stable if the restriction $R$ is 
 obeyed.\n\nhttps://indico.particle.mephi.ru/event/4/contributions/591/
LOCATION:Milan Hotel Rossini
URL:https://indico.particle.mephi.ru/event/4/contributions/591/
END:VEVENT
BEGIN:VEVENT
SUMMARY:The high-frequency gravitational waves in exact inflationary model
 s with Gauss-Bonnet term
DTSTART;VALUE=DATE-TIME:20161011T140000Z
DTEND;VALUE=DATE-TIME:20161011T141500Z
DTSTAMP;VALUE=DATE-TIME:20260814T154822Z
UID:indico-contribution-100-481@cern.ch
DESCRIPTION:Speakers: ANDREY Morozov (Bauman Moscow State Technical Univer
 sity)\, Igor Fomin (Bauman Moscow State Technical University)\nThe theory 
 of the cosmological inflation successfully describes the accelerated expan
 sion of the universe evolution at early stages. Also\, inflation in the ea
 rly universe has become the standard model for the generation of cosmologi
 cal perturbations in the universe\, the seeds for large-scale structure an
 d temperature anisotropies of the cosmic microwave background. Quantum flu
 ctuations of the inflaton field give rise to an almost scale-invariant pow
 er spectrum of cosmological perturbations.\n\nString theory is often regar
 ded as the leading candidate for unifying gravity with the other fundament
 al forces and for a quantum theory of gravity. It is known that the effect
 ive supergravity action from superstrings induces correction terms of high
 er order in the curvature\, which may play a significant role in the early
  universe. The simplest such correction is the Gauss-Bonnet term in the lo
 w-energy effective action of the string theory. Such term provides the pos
 sibility of avoiding the initial singularity of the Universe.\n\nWe consid
 er  an  action with the Gauss-Bonnet term that is coupled to a scalar fiel
 d\n\\begin{equation}\nS_{GB}=\\int d^{4}x\\sqrt{-g}\\left[\\frac{1}{2}R-\\
 frac{1}{2}(\\partial^{\\mu}\\phi\\partial_{\\mu}\\phi)-V(\\phi)-\\frac{1}{
 2}\\xi(\\phi)R^{2}_{GB}\\right]\,\n\\end{equation}\nwhere $\\phi$ is an in
 flaton field with a potential $V(\\phi)$\, $R$ is the Ricci scalar curvatu
 re of the spacetime\, $R^{2}_{\\rm GB}\n= R_{\\mu\\nu\\rho\\sigma} R^{\\mu
 \\nu\\rho\\sigma} - 4 R_{\\mu\\nu} R^{\\mu\\nu} + R^2$ is the Gauss-Bonnet
  term\, and $8\\pi G=c=1$. The Gauss-Bonnet coupling $\\xi(\\phi)$ is requ
 ired to be a function of a scalar field in order to give nontrivial effect
 s on the background dynamics.\n\nThe method of exact solutions of the back
 ground dynamical equations in a spatially flat Friedmann-Robertson-Walker 
 universe is based on the connection between Hubble parameters for inflatio
 n with Gauss-Bonnet term and standard inflation is considereded in this wo
 rk.\n\nOn the basis of this connection we calculate the exact values of th
 e parameters of cosmological perturbations at the crossing of the Hubble r
 adius for the inflationary models with Gauss-Bonnet correction.\n\nThe det
 ection of relic gravitational waves can provide the main information about
  early universe and can be used to test the theoretical models. In this co
 ntext\, it is important to develop a new methods for the detection of grav
 itational waves. One of the promising method in the high-frequency part of
  the spectrum is based on the low-frequency optical resonance phenomenon i
 n the Fabry-Perot interferometers. The description of this method and comp
 arison with another methods are also presented.\n\nhttps://indico.particle
 .mephi.ru/event/4/contributions/481/
LOCATION:Milan Hotel Rossini
URL:https://indico.particle.mephi.ru/event/4/contributions/481/
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