inflationary theory of primordial cosmological perturbation project for general relativity...
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Inflationary Theory of Primordial Cosmological
Perturbation
Project for General Relativity(Instructor: Prof.Whiting)
Sohyun Park
Brief introduction about the title
It is firmly established by observation that our universe• is homogeneous and isotropic on large scales (~
100Mpc).• has well developed inhomogeneous structure on
small scales - p.4
Mukhanov
There should be primordial perturbations to be the seeds of the structure formation! -> Inflation gives a very plausible mechanism for that!Inflationary Theory of
Primordial Cosmological Perturbation
Two systems
homogeneous, isotropic and spatially flat (zero spatial curvature) background
1st order perturbations around the inflationary background
+
Spatially flat, FRW geometry
Two functions in terms of a
Definition of Inflation : accelerated expansion
Brief History of Universe
q ~ -1 q = 1 q = 1/2 q(t_0) = -0.6
Today (t_0): inflating too, so the early one called Primordial Inflation!
Einstein eqns for FRW cosmology
Symmetry of FRW -> only two nonzero parts for stress tensor:t only
Energy density, pressure
Q) What causes inflation? See
A) ANYTHING with
How do we find something with ?
Many!, some are very complicated, but we have two simple ones:
• Positive cosmological constant
• Minimally coupled scalar with a flat potential
OK
Scalar eq for FRW
Hubble Friction
Basic inflation mechanism: particle production
Take the massless, minimally coupled scalarV=0 good approxfor flat potential
With FRW metric
Fourier transf, no coupling between different modes, consider oneAll free QFT: infinite collection of HO’s
Bunch-Davis vacuum
Basic inflation mechanism: particle production
Eq of motion
Hubble Friction
Solve it for the de Sitter case:
Solution: where
canonically normalized:
The energy of state
Now QM
?
Basic inflation mechanism: particle production
1st order Perturbations around the inflationary background
Perturbation equations
Observables: power spectra(which we can compare with data eg.CMB)
For scalar perturbations the power spectrum in the post-inflationary, radiation-dominated epoch
For metric perturbations the power spectrum
Conclusion
Inflation “washes out’’ all pre-existing classical inhomogeneities by stretching them to very large scales. It sometimes called thatInflation removes the “classical hairs.’’ However, it cannot remove Quantum fluctuations (“quantum hairs”). In place of the stretched quantum fluctuations, new ones “are generated” via the Heisenberg uncertainty relation.
-p.328 Mukhanov
The formation of our galaxy began with a quantum fluctuation…