1. Modified Gravity

2. Modification of Einstein equation replace keep diffeomorphism symmetry ! at least unimodular diffeomorphisms

3. Modification of Einstein equation modifiedgravityDarkEnergy Split is ambiguous ! example : cosmological constant

4. Quantum effective action gravitational part: functional of metric functional of metric

5. New degrees of freedom Modifications of gravity involve new degrees of freedom not necessarily new fields beyond metric what matters : degrees of freedom – not choice of field variables to describe them

6. Cosmological scalar fields Brans- Dicke theory : Quintessence : turns out to be special form of scalar model coupled to matter

7. Weyl scaling w can depend on fields !

8. Weyl scaling in Brans-Dicke theory In this version ( Einstein frame ) no modification of gravitational action !

9. Frames Jordan frame : field dependent gravitational constant ( coefficient of curvature scalar ) Jordan frame : field dependent gravitational constant ( coefficient of curvature scalar ) Einstein frame : fixed Planck mass M Einstein frame : fixed Planck mass M on level of quantum effective action: both frames are equivalent ! on level of quantum effective action: both frames are equivalent ! simply different “field – coordinates “ for solutions of differential equations simply different “field – coordinates “ for solutions of differential equations no measurement can distinguish the two frames no measurement can distinguish the two frames only dimensionless quantities can be measured only dimensionless quantities can be measured

10. Weyl scaling in matter sector fermions : constant mass in Jordan frame : field dependent mass in Einstein frame ! similar for bosons time variation of ratio nucleon mass / Planck mass: strict limits !!!

11. How to obey constraints from time variation of particle masses field dependent mass in Jordan frame field dependent mass in Jordan frame mass ~ χ in Jordan frame : constant mass in Einstein frame ! similar for bosons only tiny variation of scalar field only tiny variation of scalar field only tiny local variation of scalar field ( chameleon mechanism etc. ) only tiny local variation of scalar field ( chameleon mechanism etc. )

12. Quantum effective action with scale symmetry ( dilatation symmetry, “conformal symmetry” ) all mass scales replaced by χ only dimensionless couplings Fujii, CW potential for Higgs scalar h fixed value of

13. scalar – tensor theories violation of scale symmetry if V, F or K contain parameters with dimension of mass

14. Weyl scaling of scalar potential V’ = w 2 V cosmological constant in Jordan frame λ c in Jordan frame λ c λcλcλcλc

15. Model μ = 2  10 -33 eV m~ μ only scale :

16. Universe without Expansion

17. NATURE | NEWS Cosmologist claims Universe may not be expanding Particles' changing masses could explain why distant galaxies appear to be rushing away. Jon Cartwright 16 July 2013 German physicist stops Universe 25.07.2013

18. SonntagszeitungZuerichLaukenmann

19. The Universe is shrinking

20. The Universe is shrinking … while Planck mass and particle masses are increasing

21. What is increasing ? Ratio of distance between galaxies over size of atoms ! atom size constant : expanding geometry alternative : shrinking size of atoms general idea not new : Hoyle, Narlikar,…

22. Simple model of “ Variable Gravity Universe “ Scalar field coupled to gravity Scalar field coupled to gravity Effective Planck mass depends on scalar field Effective Planck mass depends on scalar field Simple quadratic scalar potential : Simple quadratic scalar potential : Nucleon and electron mass proportional to Planck mass Nucleon and electron mass proportional to Planck mass Neutrino mass has different dependence on scalar field Neutrino mass has different dependence on scalar field

23. Simplicity simple description of all cosmological epochs natural incorporation of Dark Energy : inflation inflation Early Dark Energy Early Dark Energy present Dark Energy dominated epoch present Dark Energy dominated epoch

24. Time history of the Universe Inflation : Universe expands Inflation : Universe expands Radiation : Universe shrinks Radiation : Universe shrinks Matter : Universe shrinks Matter : Universe shrinks Dark Energy : Universe expands Dark Energy : Universe expands

25. Compatibility with observations Almost same prediction for radiation, matter, and Dark Energy domination as Λ CDM Almost same prediction for radiation, matter, and Dark Energy domination as Λ CDM Inflation with: Inflation with: n=0.97, r=0.13 n=0.97, r=0.13 Presence of small fraction of Early Dark Energy Presence of small fraction of Early Dark Energy Large neutrino lumps Large neutrino lumps

26. Cosmon inflation Unified picture of inflation and dynamical dark energy Cosmon and inflaton are the same field

27. Quintessence Dynamical dark energy, Dynamical dark energy, generated by scalar field (cosmon ) generated by scalar field (cosmon ) C.Wetterich,Nucl.Phys.B302(1988)668, 24.9.87 P.J.E.Peebles,B.Ratra,ApJ.Lett.325(1988)L17, 20.10.87

28. Prediction : homogeneous dark energy influences recent cosmology - of same order as dark matter - Original models do not fit the present observations …. modifications

29. Merits of variable gravity model Economical setting Economical setting No big bang singularity No big bang singularity Arrow of time Arrow of time Simple initial conditions for inflation Simple initial conditions for inflation

30. Model μ = 2  10 -33 eV

31. Scalar field equation : additional force from R counteracts potential gradient : increasing χ !

32. Incoherent contribution to scalar field equation if particle mass proportional to χ :

33. Modified Einstein equation New term with derivatives of scalar field

34. Curvature scalar and Hubble parameter

35. Scaling solutions ( for constant K ) Four different scaling solutions for inflation, radiation domination, matter domination and Dark Energy domination

36. Scalar dominated epoch, inflation Universe expands for K > -4, shrinks for K -4, shrinks for K < -4.

37. No big bang singularity

38. Scaling solution is attractive

39. Scaling solution ends when K gets closer to -6

40. Radiation domination Universe shrinks !

41. Early Dark Energy Energy density in radiation increases, proportional to cosmon potential fraction in early dark energy requires large α >10

42. scaling of particle masses mass of electron or nucleon is proportional to variable Planck mass χ ! effective potential for Higgs doublet h

43. cosmon coupling to matter q χ =-(ρ-3p)/χ

44. Matter domination Universe shrinks !

45. Neutrino mass seesaw and cascademechanism omit generation structure triplet expectation value ~ doublet squared

46. Neutrino mass assume that singlet scale has not yet reached scaling limit ~ χ

47. Dark Energy domination neutrino masses scales differently from electron mass new scaling solution. not yet reached. at present : transition period

48. Why now problem Why does fraction in Dark Energy increase in present cosmological epoch, and not much earlier or much later ? neutrinos become non-relativistic at z = 5

49. Observations simplest description in Einstein frame simplest description in Einstein frame

50. Weyl scaling

51. Kinetial scalar σ with standard normalization

52. conclusions Variable gravity cosmologies can give a simple and realistic description of Universe Variable gravity cosmologies can give a simple and realistic description of Universe Compatible with tests of equivalence principle and bounds on variation of fundamental couplings if nucleon and electron masses are proportional to variable Planck mass Compatible with tests of equivalence principle and bounds on variation of fundamental couplings if nucleon and electron masses are proportional to variable Planck mass Different cosmon dependence of neutrino mass can explain why Universe makes a transition to Dark Energy domination now Different cosmon dependence of neutrino mass can explain why Universe makes a transition to Dark Energy domination now characteristic signal : neutrino lumps characteristic signal : neutrino lumps

53. f (R) - theories

54. f (R) – theories, example

55. Equivalent scalar model solve scalar field equation insert solution into effective action

56. Equivalent scalar model

57. Weyl scaling

58. Canonical scalar kinetic term

59. Expansion for small φ c = 1 : scalar mass order Planck mass, unless α is huge !!!!

60. Higher order terms in effective gravitational action similar situation if f( R ) admits Taylor expansion around R=0 similar situation if f( R ) admits Taylor expansion around R=0 additional fields with mass close to Planck mass are not relevant for late cosmology ( but inflation…) additional fields with mass close to Planck mass are not relevant for late cosmology ( but inflation…) holds also for more complicated effective actions holds also for more complicated effective actions

61. Universal coupling to massive particles Scalar field is allowed to change only by tiny amount on cosmological and local scales !

62. General f(R) theories as scalar models

63. Non – local gravity Effective Nonlocal Euclidean Gravity C. Wetterich, C. Wetterich, Gen.Rel.Grav. 30 (1998) 159

64. more general modifications of gravity can often be written in form where effective degrees of freedom are more easily visible can often be written in form where effective degrees of freedom are more easily visible massive gravity massive gravity two- metric theories two- metric theories “MOND” “MOND”

65. conclusions Modified gravity often easier understood in terms of additional fields Modified gravity often easier understood in terms of additional fields No basic distinction between modified gravity and Dark energy ( except massive gravity ) No basic distinction between modified gravity and Dark energy ( except massive gravity ) Is the picture of modified gravity useful ? Is the picture of modified gravity useful ? Sometimes, if important features are more easily visible ( scale symmetry, absence of singularities ) Sometimes, if important features are more easily visible ( scale symmetry, absence of singularities )

66. End

67. Cosmon inflation

68. Inflation : Slow roll parameters End of inflation at ε = 1

69. Number of e-foldings before end of inflation ε, η, N can all be computed from kinetial alone

70. Spectral index and tensor to scalar ratio

71. Amplitude of density fluctuations

72. Properties of density fluctuations

73. conclusion cosmon inflation : compatible with observation compatible with observation simple simple no big bang singularity no big bang singularity stability of solution singles out arrow of time stability of solution singles out arrow of time simple initial conditions simple initial conditions

74. Growing neutrino quintessence

75. connection between dark energy and neutrino properties present equation of state given by neutrino mass ! present dark energy density given by neutrino mass = 1.27

76. Neutrino cosmon coupling realized by dependence of neutrino mass on value of cosmon field realized by dependence of neutrino mass on value of cosmon field β ≈ 1 : cosmon mediated attractive force between neutrinos has similar strength as gravity β ≈ 1 : cosmon mediated attractive force between neutrinos has similar strength as gravity

77. growing neutrinos change cosmon evolution modification of conservation equation for neutrinos

78. growing neutrino mass triggers transition to almost static dark energy growingneutrinomass L.Amendola, M.Baldi,…

79. effective cosmological trigger for stop of cosmon evolution : neutrinos get non-relativistic this has happened recently ! this has happened recently ! sets scales for dark energy ! sets scales for dark energy !

80. cosmon evolution scaling “stopped”

81. neutrino lumps

82. neutrino fluctuations neutrino structures become nonlinear at z~1 for supercluster scales stable neutrino-cosmon lumps exist N.Brouzakis, N.Tetradis,… ; O.Bertolami ; Y.Ayaita, M.Weber,… D.Mota, G.Robbers, V.Pettorino, …

83. N-body code with fully relativistic neutrinos and backreaction Y.Ayaita,M.Weber,… one has to resolve local value of cosmon field and then form cosmological average; similar for neutrino density, dark matter and gravitational field

84. Formation of neutrino lumps Y.Ayaita,M.Weber,…

85. φ - dependent neutrino – cosmon coupling neutrino lumps form and are disrupted by oscillations in neutrino mass smaller backreaction

86. oscillating neutrino mass

87. oscillating neutrino lumps

88. small oscillations in dark energy

89. quantum fluctuations and dilatation anomaly

90. Dilatation anomaly Quantum fluctuations responsible both for Quantum fluctuations responsible both for fixed point and dilatation anomaly close to fxed point fixed point and dilatation anomaly close to fxed point Running couplings: hypothesis Running couplings: hypothesis Renormalization scale μ : ( momentum scale ) Renormalization scale μ : ( momentum scale ) λ~(χ/μ) –A λ~(χ/μ) –A

91. Asymptotic behavior of effective potential λ ~ (χ/μ) –A λ ~ (χ/μ) –A V ~ (χ/μ) –A χ 4 V ~ (χ/μ) –A χ 4 V ~ χ 4–A V ~ χ 4–A crucial : behavior for large χ !

92. Without dilatation – anomaly : V= const. Massless Goldstone boson = dilaton Dilatation – anomaly : V (φ ) Scalar with tiny time dependent mass : cosmon

93. Dilatation anomaly and quantum fluctuations Computation of running couplings ( beta functions ) needs unified theory ! Computation of running couplings ( beta functions ) needs unified theory ! Dominant contribution from modes with momenta ~χ ! Dominant contribution from modes with momenta ~χ ! No prejudice on “natural value “ of location of fixed point or anomalous dimension should be inferred from tiny contributions at QCD- momentum scale ! No prejudice on “natural value “ of location of fixed point or anomalous dimension should be inferred from tiny contributions at QCD- momentum scale !

94. quantum fluctuations and naturalness Jordan- and Einstein frame completely equivalent on level of effective action and field equations ( after computation of quantum fluctuations ! ) Jordan- and Einstein frame completely equivalent on level of effective action and field equations ( after computation of quantum fluctuations ! ) Treatment of quantum fluctuations depends on frame : Jacobian for variable transformation in functional integral Treatment of quantum fluctuations depends on frame : Jacobian for variable transformation in functional integral What is natural in one frame may look unnatural in another frame What is natural in one frame may look unnatural in another frame

95. quantum fluctuations and frames Einstein frame : quantum fluctuations make zero cosmological constant look unnatural Einstein frame : quantum fluctuations make zero cosmological constant look unnatural Jordan frame : quantum fluctuations can be the origin of dilatation anomaly; Jordan frame : quantum fluctuations can be the origin of dilatation anomaly; may be key ingredient for solution of cosmological constant problem ! may be key ingredient for solution of cosmological constant problem !

96. fixed points and fluctuation contributions of individual components If running couplings influenced by fixed points: individual fluctuation contribution can be huge overestimate ! here : fixed point at vanishing quartic coupling and anomalous dimension V ~ χ 4–A it makes no sense to use naïve scaling argument to infer individual contribution V ~ h χ 4

97. conclusions naturalness of cosmological constant and cosmon potential should be discussed in the light of dilatation symmetry and its anomalies naturalness of cosmological constant and cosmon potential should be discussed in the light of dilatation symmetry and its anomalies Jordan frame Jordan frame higher dimensional setting higher dimensional setting four dimensional Einstein frame and naïve estimate of individual contributions can be very misleading ! four dimensional Einstein frame and naïve estimate of individual contributions can be very misleading !

98. conclusions cosmic runaway towards fixed point may solve the cosmological constant problem solve the cosmological constant problem and and account for dynamical Dark Energy account for dynamical Dark Energy