repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf ·...

55
Repulsive gravity model for dark energy Manuel Hohmann II. Institut für theoretische Physik Foundational Aspects of Cosmology 18 February 2011 Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 1 / 31

Upload: others

Post on 24-Feb-2020

1 views

Category:

Documents


0 download

TRANSCRIPT

Page 1: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Repulsive gravity model for dark energy

Manuel Hohmann

II. Institut für theoretische Physik

Foundational Aspects of Cosmology18 February 2011

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 1 / 31

Page 2: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Outline

1 Motivation

2 Multimetric gravity

3 Multimetric cosmology

4 Simulation of structure formation

5 Solar system consistency

6 Gravitational waves

7 Conclusion

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 2 / 31

Page 3: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Outline

1 Motivation

2 Multimetric gravity

3 Multimetric cosmology

4 Simulation of structure formation

5 Solar system consistency

6 Gravitational waves

7 Conclusion

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 3 / 31

Page 4: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

The ΛCDM model of cosmology

4.6% visible matter.[Komatsu et al. ’09]

22.8% dark matter.Galaxy rotation curves.[de Blok, Bosma ’02]

Anomalous light deflection.[Wambsganss ’98]

72.6% dark energy.Accelerating expansion.[Riess et al. ’98; Perlmutter et al. ’98]

⇒ Problem: What are dark matter and dark energy?

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 4 / 31

Page 5: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

The ΛCDM model of cosmology

4.6% visible matter.[Komatsu et al. ’09]

22.8% dark matter.Galaxy rotation curves.[de Blok, Bosma ’02]

Anomalous light deflection.[Wambsganss ’98]

72.6% dark energy.Accelerating expansion.[Riess et al. ’98; Perlmutter et al. ’98]

⇒ Problem: What are dark matter and dark energy?

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 4 / 31

Page 6: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

The ΛCDM model of cosmology

4.6% visible matter.[Komatsu et al. ’09]

22.8% dark matter.Galaxy rotation curves.[de Blok, Bosma ’02]

Anomalous light deflection.[Wambsganss ’98]

72.6% dark energy.Accelerating expansion.[Riess et al. ’98; Perlmutter et al. ’98]

⇒ Problem: What are dark matter and dark energy?

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 4 / 31

Page 7: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

The ΛCDM model of cosmology

4.6% visible matter.[Komatsu et al. ’09]

22.8% dark matter.Galaxy rotation curves.[de Blok, Bosma ’02]

Anomalous light deflection.[Wambsganss ’98]

72.6% dark energy.Accelerating expansion.[Riess et al. ’98; Perlmutter et al. ’98]

⇒ Problem: What are dark matter and dark energy?

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 4 / 31

Page 8: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

The ΛCDM model of cosmology

4.6% visible matter.[Komatsu et al. ’09]

22.8% dark matter.Galaxy rotation curves.[de Blok, Bosma ’02]

Anomalous light deflection.[Wambsganss ’98]

72.6% dark energy.Accelerating expansion.[Riess et al. ’98; Perlmutter et al. ’98]

⇒ Problem: What are dark matter and dark energy?

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 4 / 31

Page 9: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

The ΛCDM model of cosmology

4.6% visible matter.[Komatsu et al. ’09]

22.8% dark matter.Galaxy rotation curves.[de Blok, Bosma ’02]

Anomalous light deflection.[Wambsganss ’98]

72.6% dark energy.Accelerating expansion.[Riess et al. ’98; Perlmutter et al. ’98]

⇒ Problem: What are dark matter and dark energy?

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 4 / 31

Page 10: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

The ΛCDM model of cosmology

4.6% visible matter.[Komatsu et al. ’09]

22.8% dark matter.Galaxy rotation curves.[de Blok, Bosma ’02]

Anomalous light deflection.[Wambsganss ’98]

72.6% dark energy.Accelerating expansion.[Riess et al. ’98; Perlmutter et al. ’98]

⇒ Problem: What are dark matter and dark energy?

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 4 / 31

Page 11: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

The ΛCDM model of cosmology

4.6% visible matter.[Komatsu et al. ’09]

22.8% dark matter?Galaxy rotation curves.[de Blok, Bosma ’02]

Anomalous light deflection.[Wambsganss ’98]

72.6% dark energy?Accelerating expansion.[Riess et al. ’98; Perlmutter et al. ’98]

⇒ Problem: What are dark matter and dark energy?

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 4 / 31

Page 12: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Explanations for the dark universe

Particle physics:Dark matter: [Bertone, Hooper, Silk ’05]

Weakly interacting massive particles (WIMPs). [Ellis et al. ’84]

Axions. [Preskill, Wise, Wilczek ’83]

Massive compact halo objects (MACHOs). [Paczynski ’86]

Dark energy: [Copeland, Sami, Tsujikawa ’06]

Quintessence. [Peebles, Ratra ’88]

K-essense. [Chiba, Okabe, Yamaguchi ’00; Armendariz-Picon, Mukhanov, Steinhardt ’01]

Chaplygin gas. [Kamenshchik, Moschella, Pasquier ’01]

Gravity:Modified Newtonian dynamics (MOND). [Milgrom ’83]

Tensor-vector-scalar theories. [Bekenstein ’04]

Curvature corrections. [Schuller, Wohlfarth ’05; Sotiriou, Faraoni ’05]

Dvali-Gabadadze-Porrati (DGP) model. [Dvali, Gabadadze, Porrati ’00, Lue ’06]

Non-symmetric gravity. [Moffat ’95]

Area metric gravity. [Punzi, Schuller, Wohlfarth ’07]

New idea: repulsive gravity⇔ negative mass!

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 5 / 31

Page 13: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Explanations for the dark universe

Particle physics:Dark matter: [Bertone, Hooper, Silk ’05]

Weakly interacting massive particles (WIMPs). [Ellis et al. ’84]

Axions. [Preskill, Wise, Wilczek ’83]

Massive compact halo objects (MACHOs). [Paczynski ’86]

Dark energy: [Copeland, Sami, Tsujikawa ’06]

Quintessence. [Peebles, Ratra ’88]

K-essense. [Chiba, Okabe, Yamaguchi ’00; Armendariz-Picon, Mukhanov, Steinhardt ’01]

Chaplygin gas. [Kamenshchik, Moschella, Pasquier ’01]

Gravity:Modified Newtonian dynamics (MOND). [Milgrom ’83]

Tensor-vector-scalar theories. [Bekenstein ’04]

Curvature corrections. [Schuller, Wohlfarth ’05; Sotiriou, Faraoni ’05]

Dvali-Gabadadze-Porrati (DGP) model. [Dvali, Gabadadze, Porrati ’00, Lue ’06]

Non-symmetric gravity. [Moffat ’95]

Area metric gravity. [Punzi, Schuller, Wohlfarth ’07]

New idea: repulsive gravity⇔ negative mass!

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 5 / 31

Page 14: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Mass in Newtonian gravity

Three types of mass! [Bondi ’57]

Active gravitational mass ma - source of gravity: φ = −GNmar .

Passive gravitational mass mp - reaction on gravity: ~F = −mp ~∇φ.Inertial mass mi - relates force to acceleration: ~F = mi~a.

Theory relates the different types of mass:

Momentum conservation: ma ∼ mp.Weak equivalence principle: mp ∼ mi .

ma ∼ mp ∼ mi experimentally confirmed.Gravity is always attractive.Convention: unit ratios and signs such that ma = mp = mi > 0.Observations exist for visible matter only.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 6 / 31

Page 15: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Mass in Newtonian gravity

Three types of mass! [Bondi ’57]

Active gravitational mass ma - source of gravity: φ = −GNmar .

Passive gravitational mass mp - reaction on gravity: ~F = −mp ~∇φ.Inertial mass mi - relates force to acceleration: ~F = mi~a.

Theory relates the different types of mass:Momentum conservation: ma ∼ mp.Weak equivalence principle: mp ∼ mi .

ma ∼ mp ∼ mi experimentally confirmed.Gravity is always attractive.Convention: unit ratios and signs such that ma = mp = mi > 0.Observations exist for visible matter only.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 6 / 31

Page 16: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Mass in Newtonian gravity

Three types of mass! [Bondi ’57]

Active gravitational mass ma - source of gravity: φ = −GNmar .

Passive gravitational mass mp - reaction on gravity: ~F = −mp ~∇φ.Inertial mass mi - relates force to acceleration: ~F = mi~a.

Theory relates the different types of mass:Momentum conservation: ma ∼ mp.Weak equivalence principle: mp ∼ mi .

ma ∼ mp ∼ mi experimentally confirmed.Gravity is always attractive.Convention: unit ratios and signs such that ma = mp = mi > 0.

Observations exist for visible matter only.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 6 / 31

Page 17: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Mass in Newtonian gravity

Three types of mass! [Bondi ’57]

Active gravitational mass ma - source of gravity: φ = −GNmar .

Passive gravitational mass mp - reaction on gravity: ~F = −mp ~∇φ.Inertial mass mi - relates force to acceleration: ~F = mi~a.

Theory relates the different types of mass:Momentum conservation: ma ∼ mp.Weak equivalence principle: mp ∼ mi .

ma ∼ mp ∼ mi experimentally confirmed.Gravity is always attractive.Convention: unit ratios and signs such that ma = mp = mi > 0.Observations exist for visible matter only.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 6 / 31

Page 18: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Dark universe from negative massIdea for dark universe: standard model with ma = mp = −mi < 0.Both copies couple only through gravity⇒ “dark”.

⇒ Preserves momentum conservation.⇒ Breaks weak equivalence principle only for cross-interaction.

Explanation of dark matter.

Explanation of dark energy.⇒ Advantage: Dark copy Ψ− of

well-known standard model Ψ+:No new parameters.No unknown masses.No unknown couplings.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 7 / 31

Page 19: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Dark universe from negative massIdea for dark universe: standard model with ma = mp = −mi < 0.Both copies couple only through gravity⇒ “dark”.

⇒ Preserves momentum conservation.⇒ Breaks weak equivalence principle only for cross-interaction.

Explanation of dark matter.

Explanation of dark energy.⇒ Advantage: Dark copy Ψ− of

well-known standard model Ψ+:No new parameters.No unknown masses.No unknown couplings.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 7 / 31

Page 20: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Dark universe from negative massIdea for dark universe: standard model with ma = mp = −mi < 0.Both copies couple only through gravity⇒ “dark”.

⇒ Preserves momentum conservation.⇒ Breaks weak equivalence principle only for cross-interaction.

Explanation of dark matter.

Explanation of dark energy.⇒ Advantage: Dark copy Ψ− of

well-known standard model Ψ+:No new parameters.No unknown masses.No unknown couplings.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 7 / 31

Page 21: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Dark universe from negative massIdea for dark universe: standard model with ma = mp = −mi < 0.Both copies couple only through gravity⇒ “dark”.

⇒ Preserves momentum conservation.⇒ Breaks weak equivalence principle only for cross-interaction.

Explanation of dark matter.

Explanation of dark energy.

⇒ Advantage: Dark copy Ψ− ofwell-known standard model Ψ+:

No new parameters.No unknown masses.No unknown couplings.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 7 / 31

Page 22: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Dark universe from negative massIdea for dark universe: standard model with ma = mp = −mi < 0.Both copies couple only through gravity⇒ “dark”.

⇒ Preserves momentum conservation.⇒ Breaks weak equivalence principle only for cross-interaction.

Explanation of dark matter.

Explanation of dark energy.

⇒ Advantage: Dark copy Ψ− ofwell-known standard model Ψ+:

No new parameters.No unknown masses.No unknown couplings.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 7 / 31

Page 23: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Dark universe from negative massIdea for dark universe: standard model with ma = mp = −mi < 0.Both copies couple only through gravity⇒ “dark”.

⇒ Preserves momentum conservation.⇒ Breaks weak equivalence principle only for cross-interaction.

Explanation of dark matter.

Explanation of dark energy.⇒ Advantage: Dark copy Ψ− of

well-known standard model Ψ+:No new parameters.No unknown masses.No unknown couplings.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 7 / 31

Page 24: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Repulsive Einstein gravity

Positive and negative test masses follow different trajectories.Two types of test mass trajectories⇒ two types of observers.Observer trajectories are autoparallels of two connections ∇±.Observers attach parallely transported frames to their curves.Frames are orthonormalized using two metric tensors g±ab.

No-go theorem forbids bimetric repulsive gravity. [MH, M. Wohlfarth ’09]

Solution: N ≥ 3 metrics gIab and standard model copies ΨI .

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 8 / 31

Page 25: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Repulsive Einstein gravity

Positive and negative test masses follow different trajectories.Two types of test mass trajectories⇒ two types of observers.Observer trajectories are autoparallels of two connections ∇±.Observers attach parallely transported frames to their curves.Frames are orthonormalized using two metric tensors g±ab.No-go theorem forbids bimetric repulsive gravity. [MH, M. Wohlfarth ’09]

Solution: N ≥ 3 metrics gIab and standard model copies ΨI .

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 8 / 31

Page 26: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Outline

1 Motivation

2 Multimetric gravity

3 Multimetric cosmology

4 Simulation of structure formation

5 Solar system consistency

6 Gravitational waves

7 Conclusion

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 9 / 31

Page 27: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Construction principles

1. N ≥ 3 copies of standard model matter ΨI , I = 1, . . . ,N.2. N metric tensors gI

ab.3. Each standard model copy ΨI couples only to its metric gI .

⇒ SM [gI ,ΨI ] =

∫d4x

√gILM [gI ,ΨI ] .

4. Different sectors couple only gravitationally.

⇒ S = SG[g1, . . . ,gN ] +N∑

I=1

SM [gI ,ΨI ] .

5. Field equations contain at most second derivatives of the metrics.6. Symmetric with respect to permutations of the sectors (gI ,ΨI).

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 10 / 31

Page 28: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Action and equations of motion

Gravitational action:

SG[g1, . . . ,gN ] =12

∫d4x√

g0

N∑I,J=1

(x + yδIJ)gIijRJij + F (SIJ)

.Symmetric volume form g0 = (g1g2 . . . gN)1/N .F (SIJ) quadratic in connection difference tensors SIJ = ΓI − ΓJ .

⇒ Equations of motion:

T Iab =

√g0

gI

− 12N

gIab

N∑J,K=1

(x + yδJK )gJijRKij +

N∑J=1

(x + yδIJ)RJab

+ terms linear in ∇ISJK

+ terms quadratic in SIJ .

⇒ Repulsive Newtonian limit for N ≥ 3.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 11 / 31

Page 29: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Action and equations of motion

Gravitational action:

SG[g1, . . . ,gN ] =12

∫d4x√

g0

N∑I,J=1

(x + yδIJ)gIijRJij + F (SIJ)

.Symmetric volume form g0 = (g1g2 . . . gN)1/N .F (SIJ) quadratic in connection difference tensors SIJ = ΓI − ΓJ .

⇒ Equations of motion:

T Iab =

√g0

gI

− 12N

gIab

N∑J,K=1

(x + yδJK )gJijRKij +

N∑J=1

(x + yδIJ)RJab

+ terms linear in ∇ISJK

+ terms quadratic in SIJ .

⇒ Repulsive Newtonian limit for N ≥ 3.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 11 / 31

Page 30: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Outline

1 Motivation

2 Multimetric gravity

3 Multimetric cosmology

4 Simulation of structure formation

5 Solar system consistency

6 Gravitational waves

7 Conclusion

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 12 / 31

Page 31: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Cosmological symmetry

Standard cosmology: Robertson–Walker metrics

gI = −n2I (t)dt ⊗ dt + a2

I (t)γαβdxα ⊗ dxβ .

Lapse functions nI .Scale factors aI .Spatial metric γαβ of constant curvature k ∈ {−1,0,1} andRiemann tensor R(γ)αβγδ = 2kγα[γγδ]β .

Perfect fluid matter:

T I ab = (ρI + pI)uIauIb + pIgIab .

Normalization: gIabuIauIb = −1.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 13 / 31

Page 32: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Simple cosmological model

Early universe: radiation; late universe: dust.Copernican principle: common evolution for all matter sectors.

⇒ Single effective energy-momentum tensor T Iab = Tab.

⇒ Single effective metric gIab = gab.

⇒ Common scale factors aI = a and lapse functions nI = n.⇒ Rescale cosmological time to set n ≡ 1.⇒ Ricci tensors RI

ab = Rab become equal.⇒ Connection differences SIJ i

jk = 0 vanish.⇒ Equations of motion simplify for repulsive Newtonian limit:

(2− N)Tab = Rab −12

Rgab .

⇒ Negative effective gravitational constant for early / late universe.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 14 / 31

Page 33: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Simple cosmological model

Early universe: radiation; late universe: dust.Copernican principle: common evolution for all matter sectors.

⇒ Single effective energy-momentum tensor T Iab = Tab.

⇒ Single effective metric gIab = gab.

⇒ Common scale factors aI = a and lapse functions nI = n.⇒ Rescale cosmological time to set n ≡ 1.⇒ Ricci tensors RI

ab = Rab become equal.⇒ Connection differences SIJ i

jk = 0 vanish.

⇒ Equations of motion simplify for repulsive Newtonian limit:

(2− N)Tab = Rab −12

Rgab .

⇒ Negative effective gravitational constant for early / late universe.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 14 / 31

Page 34: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Simple cosmological model

Early universe: radiation; late universe: dust.Copernican principle: common evolution for all matter sectors.

⇒ Single effective energy-momentum tensor T Iab = Tab.

⇒ Single effective metric gIab = gab.

⇒ Common scale factors aI = a and lapse functions nI = n.⇒ Rescale cosmological time to set n ≡ 1.⇒ Ricci tensors RI

ab = Rab become equal.⇒ Connection differences SIJ i

jk = 0 vanish.⇒ Equations of motion simplify for repulsive Newtonian limit:

(2− N)Tab = Rab −12

Rgab .

⇒ Negative effective gravitational constant for early / late universe.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 14 / 31

Page 35: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Cosmological equations of motion

Insert Robertson–Walker metric into equations of motion:

ρ =3

2− N

(a2

a2 +ka2

),

p = − 12− N

(2

aa

+a2

a2 +ka2

).

⇒ Positive matter density ρ > 0 requires k = −1 and a2 < 1.⇒ No solutions for k = 0 or k = 1.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 15 / 31

Page 36: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Accelerating expansion

Acceleration equation:

aa

=N − 2

6(ρ+ 3p) .

Factor N − 2 > 0 for multimetric gravity.Strong energy condition(

Tab −12

Tgab

)tatb ≥ 0

for all timelike vector fields ta implies ρ+ 3p ≥ 0.⇒ Acceleration must be positive.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 16 / 31

Page 37: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Explicit solution

Equation of state: p = ωρ; dust: ω = 0, radiation: ω = 1/3.General solution using conformal time η defined by dt = a dη:

a = a0

(cosh

(3ω + 1

2(η − η0)

)) 23ω+1

,

ρ =3

(N − 2)a20

(cosh

(3ω + 1

2(η − η0)

))− 6ω+63ω+1

.

-15 -10 -5 5 10 15

t

a0

5

10

15

a

a0

-4 -2 2 4

t

a0

0.2

0.4

0.6

0.8

1.0

Ρ

Ρ0

⇒ Big bounce at η = η0. [MH, M. Wohlfarth ’10]

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 17 / 31

Page 38: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Outline

1 Motivation

2 Multimetric gravity

3 Multimetric cosmology

4 Simulation of structure formation

5 Solar system consistency

6 Gravitational waves

7 Conclusion

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 18 / 31

Page 39: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Ingredients

1. Metrics gIab = g0

ab + hIab with

g0 = −dt ⊗ dt + a2(t)γαβdxα ⊗ dxβ

and a(t) determined by cosmology.2. Scale for structure formation� curvature radius of the universe:

Cubic volume 0 ≤ xα ≤ `.Approximate γαβ by δαβ .Periodic boundary conditions.

3. Matter content: n point masses M for each sector.Model for dust matter: p = 0.Matter density:

ρ =Mn

(a`)3 .

4. Large mean distance a`/ 3√

Nn� 2GM.5. Small velocities |vαIi | = |axαIi | � 1.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 19 / 31

Page 40: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Evolution of structures for all matter types

N = 4.n = 16384.7.5 daysCPU time.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 20 / 31

Page 41: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Final state for one matter type

Galacticclusters.Empty voids.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 21 / 31

Page 42: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Outline

1 Motivation

2 Multimetric gravity

3 Multimetric cosmology

4 Simulation of structure formation

5 Solar system consistency

6 Gravitational waves

7 Conclusion

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 22 / 31

Page 43: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Physical situation in the solar system

Consider only repulsive gravity between different sectors.⇒ Different matter types should separate.⇒ Energy-momentum tensor contains only visible matter:

⇒ T+ab = T 1

ab 6= 0.⇒ T−

ab = T 2ab = . . . = T N

ab = 0.

Permutation symmetry between sectors.

⇒ Visible matter has equal effects on all dark sectors.⇒ Metric:

⇒ g+ab = g1

ab.⇒ g−

ab = g2ab = . . . = gN

ab.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 23 / 31

Page 44: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Physical situation in the solar system

Consider only repulsive gravity between different sectors.⇒ Different matter types should separate.⇒ Energy-momentum tensor contains only visible matter:

⇒ T+ab = T 1

ab 6= 0.⇒ T−

ab = T 2ab = . . . = T N

ab = 0.

Permutation symmetry between sectors.⇒ Visible matter has equal effects on all dark sectors.⇒ Metric:

⇒ g+ab = g1

ab.⇒ g−

ab = g2ab = . . . = gN

ab.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 23 / 31

Page 45: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Parametrized post-Newtonian formalism

Characterize single-metric gravity theories by 10 parameters.[Thorne, Will ’71; Will ’93]

2 parameters can be obtained from linearized field equations.Values constrained by experiment, e.g., γ = 1± 2.3 · 10−5.

Extension of PPN formalism for multimetric gravity theories.[MH, M. Wohlfarth ’10]

Extended set of 26 PPN parameters.8 parameters can be obtained from linearized field equations.10 parameters correspond to single-metric parameters⇒experimentally measured.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 24 / 31

Page 46: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Parametrized post-Newtonian formalism

Characterize single-metric gravity theories by 10 parameters.[Thorne, Will ’71; Will ’93]

2 parameters can be obtained from linearized field equations.Values constrained by experiment, e.g., γ = 1± 2.3 · 10−5.Extension of PPN formalism for multimetric gravity theories.[MH, M. Wohlfarth ’10]

Extended set of 26 PPN parameters.8 parameters can be obtained from linearized field equations.10 parameters correspond to single-metric parameters⇒experimentally measured.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 24 / 31

Page 47: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

PPN consistent theory

Consider gravitational action of the form:

SG =12

∫d4x√

g0

N∑I=1

gI ij

[zSI

k SI kij + uSI

i SIj +

N∑J=1

(x + yδIJ)RJij

].

Parameters in the action:

x =1

8− 4N, y =

4− N8− 4N

, z = − 4− N8− 4N

, u = −12− 3N8− 4N

.

⇒ PPN parameters from linearized formalism:α+ = 1, θ+ = 0: standard PPN gauge choice.γ+ = 1, σ+

+ = −2: experimental consistency.α− = −1: repulsive Newtonian limit.γ− = −1, θ− = 0, σ−

+ = 2: additional “dark” PPN parameters.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 25 / 31

Page 48: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Outline

1 Motivation

2 Multimetric gravity

3 Multimetric cosmology

4 Simulation of structure formation

5 Solar system consistency

6 Gravitational waves

7 Conclusion

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 26 / 31

Page 49: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Propagation velocity

Write linearized vacuum field equations as:

N∑J=1

DIJab

cdhJcd = 0 .

Differential operator D.Consider wavelike solution:

hIab = hI 0

abeikaxa.

Multiplication operator D.Non-vanishing solution require zero eigenvalue of D.det D ∝ (kaka)10.

⇒ Solutions exist only for kaka = 0.⇒ Gravitational waves are null.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 27 / 31

Page 50: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Polarization and E(2) class

Up to 6 polarizations in general metric theories.Theories classified by representations of E(2).E(2) class of multimetric gravity depends on 3 parameters:

P6=0ssfffffffffffff

=0++WWWWWWWWWWWWWWW

P + 2R=0uullllll 6=0

))RRRRRR M6=0wwoooooo =0

&&NNNNNN

N2 N3 III5 II6

2 tensors +1 scalar +2 vectors +1 scalar

PPN consistent theory shown before of class N2.⇒ Same class as general relativity.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 28 / 31

Page 51: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Outline

1 Motivation

2 Multimetric gravity

3 Multimetric cosmology

4 Simulation of structure formation

5 Solar system consistency

6 Gravitational waves

7 Conclusion

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 29 / 31

Page 52: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Summary

ΛCDM model describes our universe.Constituents of dark matter & dark energy are unknown.

Idea here: Dark universe might be explained by repulsive gravity.⇒ Repulsive gravity requires an extension of general relativity.⇒ No-go theorem: bimetric repulsive gravity is not possible.⇒ Multimetric repulsive gravity with N ≥ 3 by explicit construction.⇒ Cosmology features late-time acceleration and big bounce.⇒ Structure formation features clusters and voids.⇒ Repulsive gravity is consistent with solar system experiments.⇒ Gravitational waves are null.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 30 / 31

Page 53: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Summary

ΛCDM model describes our universe.Constituents of dark matter & dark energy are unknown.Idea here: Dark universe might be explained by repulsive gravity.

⇒ Repulsive gravity requires an extension of general relativity.⇒ No-go theorem: bimetric repulsive gravity is not possible.⇒ Multimetric repulsive gravity with N ≥ 3 by explicit construction.⇒ Cosmology features late-time acceleration and big bounce.⇒ Structure formation features clusters and voids.⇒ Repulsive gravity is consistent with solar system experiments.⇒ Gravitational waves are null.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 30 / 31

Page 54: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Outlook

Remaining PPN parameters should be determined from fullmultimetric PPN formalism.Restrict multimetric gravity theories by additional PPN bounds.Establish further construction principles, e.g., continuoussymmetry between sectors.Examine initial-value problem.Determine further exact solutions (single point mass. . . ).Advanced simulation of structure formation includingthermodynamics using GADGET-2 (Millenium Simulation).Search for repulsive gravity sources in the galactic voids throughgravitational lensing.Application to binaries: gravitational radiation should be emitted inall sectors, but only one type is visible.

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 31 / 31

Page 55: Repulsive gravity model for dark energykodu.ut.ee/~manuel/talks/multi/2011_02_18_hamburg.pdf · 2017-06-09 · Repulsive gravity model for dark energy Manuel Hohmann II. Institut

Outlook

Remaining PPN parameters should be determined from fullmultimetric PPN formalism.Restrict multimetric gravity theories by additional PPN bounds.Establish further construction principles, e.g., continuoussymmetry between sectors.Examine initial-value problem.Determine further exact solutions (single point mass. . . ).Advanced simulation of structure formation includingthermodynamics using GADGET-2 (Millenium Simulation).Search for repulsive gravity sources in the galactic voids throughgravitational lensing. Prediction!Application to binaries: gravitational radiation should be emitted inall sectors, but only one type is visible. Prediction!

Manuel Hohmann (Uni Hamburg) Repulsive gravity & cosmology FAC 2011 31 / 31