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P. Pasipoularides in Collaboration with K. Farakos (NTUA) and

THESSALONIKI 2008, NEB XIII RECENT DEVELOPMENTS IN GRAVITY. Title: BULK PHOTONS IN ASYMMETRICALLY WARPED SPACETIMES. P. Pasipoularides in Collaboration with K. Farakos (NTUA) and N. Mavromatos (Kings ‘ s College London). BRANE WORLD MODELS.

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P. Pasipoularides in Collaboration with K. Farakos (NTUA) and

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  1. THESSALONIKI 2008, NEB XIII RECENT DEVELOPMENTS IN GRAVITY Title: BULK PHOTONS IN ASYMMETRICALLY WARPED SPACETIMES P. Pasipoularides in Collaboration with K. Farakos (NTUA) and N. Mavromatos (Kings ‘s College London)

  2. BRANE WORLD MODELS • Theorists, in an attempt to solve the hierarchy problem, invented new phenomenological models with extra dimensions, which are known as brane world models (non stringy brane models). • Brane models give new physics and predictions in: • Astrophysics and cosmology • Modifications to Newtons Law (r~160μm) • High energy particle physics (1TeV-10TeV LHC)

  3. BRANE WORLD MODELS • Our world is trapped in a three dimensional brane which is embedded in a multidimensional space (BULK) • Only gravitons can propagate in the bulk , hence only gravitons possess KK excitations. • However, beyond the standard brane world scenario, there are other models where standard model particles, or some of standard model particles, can live in the bulk. Bulk Bulk Brane z (extra dimension)

  4. BRANE WORLD MODELS • LARGE EXTRA DIMENSIONS(R≤160μm) : ADD Model(I. Antoniadis, Arkani-Hammed, Dimopoulos and Dvali). Flat space-time. • INFINITE EXTRA DIMENSIONS: SECOND RANDALL-SUNDRUM MODEL. (but there is an effective size for the extra dimension due to the curvature of the extra space) • SMALL EXTRA DIMENSIONS (r~10^(-33)cm): FIRST RANDALL-SUNDRUM MODEL. (Bulk Gauge fields and fermions, Higgs field Localized on the negative tension brane)

  5. FIRST RANDALL-SUNDRUM MODEL SMorVisiblebrane Planck orHidden brane

  6. FIRST RANDALL-SUNDRUM MODEL • The RS metric is a solution of the Einstein equations only when the following fine-tuning is satisfied. • The induced metric on the brane is Minkowski. • The RS metric preserves 4D Lorentz invariance in the bulk.

  7. ASYMMETRYCALLY WARPED SPACETIMES • Beyond the Randall-Sundrum metric we can assume a more general answatz: • If thespace and time warp factors are different the 5D spacetime is called asymmetrically warped

  8. ASYMMETRICALLY WARPED SPACETIMES The induced metric on the brane(z=0)is Minkowski if we assume that However, 4D Lorentz invariance is violated in the Bulk, due to the difference between the space and time warp factors.

  9. ASYMMETRICALLY WARPED SPACETIMES • Asymmetrically warped Static solutions: • M. Visser, Physics Letters B159, 22-25 (1985). • Csaba Csaki, Joshua Erlich and Christophe Grojean, Nucl.Phys.B604:312-342,2001. • S.L. Dubovsky, JHEP 0201:012,2002. • Peter Bowcock, Christos Charmousis and Ruth Gregory, Class.Quant.Grav.17:4745-4764,2000. • Extra matter in the bulk is necessary otherwise the Einstein equation is not satisfied by the assymetrically warped static solutions

  10. ASYMMETRICALLY WARPED SPACETIMES Cosmological evolution reasons for asymmetrically warped brane models • Static solutions like that of RS-Model can be used as background approximately only for a short period of time around our epoch t=t0. For larger periods of time the complete cosmological evolution must be taken into account. • The corresponding static solution is obtained if we set t=t0 In general we expect different warp factors in our epoch • Daniel J.H. Chung, Edward W. Kolb and Antonio Riotto, Phys.Rev.D65:083516,2002

  11. BRANE AND BULK FIELDS IN ASYMMETRICALLY WARPED SPACETIMES • Brane fields (completely pinned on the brane) can not “see” the difference between the warp factors. The space-time for these field is Minkowski. • Bulk fields are described by a wave function. Due to the extension of the wave function in the bulk the bulk field “sees” the difference between the warp factors and 4D Lorenzt symmetry is violated.

  12. ASYMMETRICALLY WARPED SPACETIMES Gravitational violation of Lorentz symmetry. Direct signal from superluminous propagation of gravitational waves. Gravitons traveling in the bulk Photons pinned on the brane extra dimension z

  13. ASYMMETRICALLY WARPED SPACETIMES AdS-Reissner Nordstrom Black Hole Solution μand Q are the mass and charge of the five dimensional AdS Black Hole

  14. ASYMMETRICALLY WARPED SPACETIMES AdS-Reissner Nordstrom Black Hole Solution as a linearized perturbation around the RS-metric.

  15. ASYMMETRICALLY WARPED SPACETIMES Ads RN Black Hole metric as a linearized perturbation around the RS-metric. We assume that δh(z) is small everywhere in the bulk We consider Z2 symmetry and a second brane at the position z=zc, in order to achieve the structure (S1/Z2) of the first RS-model.

  16. BULK PHOTONS IN ASYMMETRICALLY WARPED SPACETIMES • We aim to study bulk photons in an asymmetrically warped spacetime which is a linear perturbation around the RS metric.

  17. BULK PHOTONS IN ASYMMETRICALLY WARPED SPACETIMES Equation of motion in the case of 5D U(1) Gauge fields Plane wave Answatz

  18. BULK PHOTONS IN ASYMMETRICALLY WARPED SPACETIMES If we use the formulation of time independent perturbation theory we obtain: Boundary Condition on the brane

  19. BULK PHOTONS IN ASYMMETRICALLY WARPED SPACETIMES Photons in the case of the RS1-model Unperturbed Equation Zero Mode plus Discrete Spectrum

  20. BULK PHOTONS IN ASYMMETRICALLY WARPED SPACETIMES Time independent perturbation theory: Zero mode Zero order First order correction Second order correction

  21. BULK PHOTONS IN ASYMMETRICALLY WARPED SPACETIMES Energy dependent phase and group velocity of light

  22. BULK PHOTONS IN ASYMMETRICALLY WARPED SPACETIMES Final Formulas for phase and group velocity of light when βG<<1 Quadratic dependence on the energy

  23. Our main result is a subluminous effective refractive index for vacuum We see that, photons with different energies propagate with different velocities. Hence, we will observe a time lag of the arrival times of photons, which were emitted simultaneously by a remote astrophysical source. In particular photons with smaller energies will arrive first, and photons with larger energies will follow.

  24. COMPARING WITH THE EXPERIMENTAL DATA OF MAGIC Magic is an imaging atmospheric Cherenkov telescope which can detect very high energy electromagnetic particles (VHE), in particular gamma rays. VHE photons have energies between 0.1TeV-30TeV. They are photons from conversion of gravitational Energy, when a very massive rotating star is collapsing to a supermassive black hole (Blazar or AGN).

  25. 150-250 GeV Magic observations during a flare (which lasts twenty minutes) of the nearby blazar (AGN) Markarian 501 ( Z=0.034), in July 9 (2005), indicates a 4±1 min time delay between the peaks of the time profile envelops for photons with energies smaller than ω<0.25 TeVand photons with ω>1.2 TeV 250-600 GeV 4 mins-bins 600-1200 GeV 1.2-10 TeV J. Albert et al, astro-ph/070008

  26. COMPARING WITH THE EXPERIMENTAL DATA OF MAGIC Possible interpretations of delays of more energetic photons • It is an energy dependent effect in the source (SSC mechanism). • New physics induces an effective refractive index for vacuum. • Most of Quantum Gravity Models seem to predict a dispersion relation for vacuum. • Or may be brane models with Bulk photons and an assymetrically warped metric (especially in our model we have quadratic prediction for the refractive index).

  27. COMPARING WITH THE EXPERIMENTAL DATA OF MAGIC A numerical analysis based on Magic results, which aim at the reconstruction of the original electromagnetic pulse maximizing its energy, assuming a refractive index for vacuum (two cases linear and quadratic): predicts the following values for the two mass scales MAGIC Coll. & Ellis, Mavromatos, Nanopoulos, Sakharov, Sarkisyan, arXive: 07082889 [astro-ph]

  28. COMPARING WITH THE EXPERIMENTAL DATA OF MAGIC Theoretical analysis: Brane Models Numerical analysis: Magic results fitting

  29. COMPARING WITH THE EXPERIMENTAL DATA OF MAGIC We compute numerically the parameter βG AdS-Schwarzchild Black Hole Solution AdS-Reissner Nordstrom Black Hole Solution Average deviation around the RS1-Metric

  30. COMPARING WITH THE MAGIC EXPERIMENT The small values we obtain for <δh> are consistent with the weak nature of the perturbation

  31. CONCLUSIONS • We study asymmetrically warped brane models with bulk photons. We show that the standard Lorentz invariant dispersion relation for 4D photons, possesses nonlinear corrections which lead to an Energy-dependent speed of light. • We compared with the experimental data of Magic and we set concrete restrictions to the specific brane models we examined. • We propose further investigation for other types of particles such as, gravitons and fermions. Similar dispersion relations are expected.

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