The Cosmological Slingshot The Cosmological Slingshot Scenario Scenario A New Proposal for Early Time A New Proposal for Early Time Cosmology Cosmology Germani, NEG, Kehagias, hep-th/0611246 Germani, NEG, Kehagias, arXiv:0706.0023 Germani, Ligouri, arXiv:0706.0025
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The Cosmological Slingshot The Cosmological Slingshot ScenarioScenario
A New Proposal for Early Time A New Proposal for Early Time CosmologyCosmology
Germani, NEG, Kehagias, hep-th/0611246
Germani, NEG, Kehagias, arXiv:0706.0023
Germani, Ligouri, arXiv:0706.0025
Standard cosmologyStandard cosmologyIt is nearly It is nearly
homogeneous homogeneous It is nearly It is nearly isotropicisotropic
The vacuum The vacuum energy density energy density is very smallis very small
It is expanding It is expanding It is It is acceleratingaccelerating
The space is The space is almost flatalmost flat
The perturbations around The perturbations around homogeneity have a flat homogeneity have a flat (slightly red) spectrum(slightly red) spectrum
Space curvature+1, 0
4d metric
Cosmic time
Scale factor
Space Coordinate
s(polar)
What do we What do we know about know about
the universe?the universe?
WMAP collaboration
astro-ph/0603449
Standard cosmologyStandard cosmologyIt is nearly It is nearly
homogeneous homogeneous It is nearly It is nearly isotropicisotropic
The vacuum The vacuum energy density energy density is very smallis very small
It is expanding It is expanding It is It is acceleratingaccelerating
The space is The space is almost flatalmost flat
4d metric
Einstein equationsHubble equation
Energy density
Curvature term
Equation of state
The perturbations around The perturbations around homogeneity have a flat homogeneity have a flat (slightly red) spectrum(slightly red) spectrum
Energy Conditions
Equation of state
Standard cosmologyStandard cosmologyIt is nearly It is nearly
homogeneous homogeneous It is nearly It is nearly isotropicisotropic
The vacuum The vacuum energy density energy density is very smallis very small
It is expanding It is expanding It is It is acceleratingaccelerating
The space is The space is almost flatalmost flat
4d metric
Hubble equation
to
a
t
Plank
tPlank
Big
Bang
Solution
The perturbations around The perturbations around homogeneity have a flat homogeneity have a flat (slightly red) spectrum(slightly red) spectrum
Standard cosmologyStandard cosmologyIt is nearly It is nearly
homogeneous homogeneous It is nearly It is nearly isotropicisotropic
The vacuum The vacuum energy density energy density is very smallis very small
It is expanding It is expanding It is It is acceleratingaccelerating
The space is The space is almost flatalmost flat
tot
tPlank
The perturbations around The perturbations around homogeneity have a flat homogeneity have a flat (slightly red) spectrum(slightly red) spectrum
is constant in the observable region of 1028 cm
Causally disconnected regions are in equilibrium!
Standard cosmologyStandard cosmologyIt is nearly It is nearly
homogeneous homogeneous It is nearly It is nearly isotropicisotropic
The vacuum The vacuum energy density energy density is very smallis very small
It is expanding It is expanding It is It is acceleratingaccelerating
The space is The space is almost flatalmost flat
The perturbations around The perturbations around homogeneity have a flat homogeneity have a flat (slightly red) spectrum(slightly red) spectrum
Isotropic solutions form a subset of measure zero on the
set of all Bianchi solutions
Perturbations around isotropy dominate at early time, like a -