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Gravity in Higgs phase

Gravity in Higgs phase. Shinji Mukohyama IPMU, U of Tokyo. Arkani-Hamed, Cheng, Luty and Mukohyama, JHEP 0405:074,2004. Arkani-Hamed, Cheng, Luty and Mukohyama and Wiseman, JHEP 0701:036,2007. Mukohyama, JCAP 0610:011,2006. Can we change gravity in IR?.

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Gravity in Higgs phase

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  1. Gravity in Higgs phase Shinji MukohyamaIPMU, U of Tokyo • Arkani-Hamed, Cheng, Luty and Mukohyama, JHEP 0405:074,2004. • Arkani-Hamed, Cheng, Luty and Mukohyama and Wiseman, JHEP 0701:036,2007. • Mukohyama, JCAP 0610:011,2006.

  2. Can we change gravity in IR? • Change Theory? (eg. Massive gravity, DGP model)

  3. 4D GR length scale Need UVcompletion lPl Exactly 4D GR microscopic UV scale Massive gravity & DGP model 1000km H0-1 length scale Need UVcompletion Look like4D GR Modified gravityin IR

  4. Can we change gravity in IR? • Change Theory?(eg. Massive gravity, DGP model) Macroscopic UV scalesCannot be decoupled • Change State?Higgs phase of gravityThe simplest: Ghost condensationArkani-Hamed, Cheng, Luty and Mukohyama, JHEP 0405:074,2004.

  5. Higgs mechanism • Spontaneously breaks gauge symmetry. (Theory itself has gauge symmetry.) • Gives mass to gauge boson. • Changes Gauss law to Yukawa law! • Can describe weak interaction!

  6. Ghost condensation Arkani-Hamed, Cheng, Luty and Mukohyama, JHEP 0405:074,2004 • Spontaneously breaks Lorentz symmetry. (Theory itself has Lorentz symmetry.) • Gives “mass” to graviton. • Adds oscillating time-dependent potential to Newton potential! (But the time scale is very long.) = Higgs phase of gravity

  7. Bounds on symmetry breaking scale M Arkani-Hamed, Cheng, Luty and Mukohyama and Wiseman, JHEP 0701:036,2007 M 0 100GeV 1TeV allowed ruled out Jeans Instability(sun) ruled out Twinkling from Lensing(CMB) ruled out Supernova time-delay So far, there is no conflict with experiments and observations if M < 100GeV.

  8. For simplicity in FRW universe Ghost condensateis an attractor! EOM is or Ghosty

  9. Can be an alternative to DE and DM? Usual Higgs mechanism Yes, at least forFRW background! L=0 L=0 “OK” for linear perturbation! Present value DE likecomponent DM likecomponent Very interestingnon-linear dynamics Condensate

  10. effective mB redshift Geometrical properties Linear Perturbation Input H(z) & rvis(z) Mukohyama, JCAP 0610:011,2006. Higgs sector Lagrangian Output Linear perturbation equation Compare! Dynamical properties

  11. Simplest case • Exact shift symmetry, i.e. no potential • May be called LGDM. (FRW evolution is exactly like LCDM.) • Linear perturbation equation(derived using the formalism in Mukohyama, JCAP 0610:011,2006)

  12. Summary • Ghost condensation is the simplest Higgs phase of gravity. • The low-E EFT is determined by the symmetry breaking pattern. No ghost in the EFT. • Gravity is modified in IR. • Consistent with experiments and observations if M < 100GeV. • Behaves like DE+DM for FRW background and large-scale linear perturbation. • The simplest case is LGDM. • Cosmological perturbation may distinguish ghost condensation from DE/DM.

  13. Thank you very much!

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