Conservation of the non linear curvature perturbation in generic single field inflation
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Conservation of the non-linear curvature perturbation in generic single-field inflation. Yukawa Institute for Theoretical Physics Atsushi Naruko. In Collaboration with Misao Sasaki Based on : Class. Quantum Grav. 28 072001. The contents of talk.

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Conservation of the non linear curvature perturbation in generic single field inflation

Conservation of the non-linear curvature perturbation in generic single-field inflation

Yukawa Institute for Theoretical Physics

Atsushi Naruko

In Collaboration with Misao Sasaki

Based on : Class. Quantum Grav. 28 072001


The contents of talk
The contents of talk

1, curvature perturbation and non-Gaussianity

2, gradient expansion approach

3, conservation of non-linear curvature perturbation

3.1, G = 0 (for canonical, k-essential scalar)

3.2, G ≠ 0 (for Galileon scalar) in Einstein gravity

4, summary


curvature perturbation

and

non-Gaussianity


Curvature perturbation
Curvature perturbation

  • Curvature perturbation on a slicing is regarded as Newton

    potential, therefore it gives the initial condition for

    Cosmic Microwave Background (CMB).

  • Through the observations of CMB, there is a possibility that

    we can subtract the information of primordial universe.

  • Recently, a lot of attention is paid to “non-Gaussianity” in CMB

    as a new window for primordial universe.


Non gaussianity
Non-Gaussianity

  • From the observation by WMAP, we know that

    temperature fluctuations in CMB are scale invariant and

    are Gaussianly distributed.

  • We parameterise the deviation from Gaussian using “fNL”

  • The three point function is sensitive to this type NG.



Non linear cosmological perturbations
non-linear cosmological perturbations

  • In order to estimate the non-Gaussianity correctly,

    we have to make a analysis beyond linear order.

  • There are mainly two approaches to nonlinear

    cosmological perturbations.

    1. the standard perturbative approach.

    2. the gradient expansion approach

  • In the gradient expansion, the field equations are expanded

    in powers of spatial gradients, therefore, it is applicable

    only to perturbations on superhorizon scales.

    → However, the full nonlinear effects are taken into account.


Outside horizon
Outside Horizon

  • Thanks to the talk by Yamaguchi-san,

    Mizuno-san and De Felice-san,

    we know well about the perturbation

    in Galileon field at horizon exit.

inflation

  • To give a theoretical prediction precisely , we need to solve

  • the evolution of curvature perturbation outside Horizon.

  • It have been known that curvature perturbation is conserved

  • on superhorizon scales in the case of ◯◯◯ under ◎◎◎.


Lyth malik and sasaki
Lyth, Malik and sasaki

JCAP 0505:004,2005.

  • Let’s consider a perfect fluid :

and write down the energy conservation law,

  • We take uniform energy density slicing

the rhs become a function of t

if P is the function of ρ

curvature per. is conserved


P = P (ρ) ?

  • From the study by LMS, we know that if P is afunction of ρ,

    curvature perturbation is conserved on uniform energy density

    slice regardless of gravity theory.

  • In the case of scalar field, whether / when this condition is

    satisfied is not so trivial because the relation between P and ρ

    is complicated.

canonical :

k-essence :

Galileon : very much complicated…


Our goal
Our goal

  • We investigate the evolution of curvature perturbation

    on superhorizon scales in rather generic single-feild inflation

    using gradient expansion approach.

  • We show the conservation of non-linear curvature perturbation

    by using scalar field equation.

  • We clarify under which circumstances curvature perturbation

    is conserved in the case of scalar field.


Conservation

of

curvature perturbation


Metric
metric

  • We express the metric in the (3 + 1) form,

  • We choose the spatial coordinate such that βi vanish

  • and further decompose the spatial metric as

  • Ψ is called as curvature perturbation because it corresponds

  • to 3D-ricci scalar at leading order in gradient expansion.

  • We define the expansion by the divergence of nμ ,

  • which is a vector orthogonal to t = const. surface.

t = const.


Scalar field equation
scalar field equation

  • We consider a rather generic scalar field.

  • canonical

  • K-essence, DBI

Galileon

  • After taking the variation of the above action, we obtain

  • the scalar field equation


G = 0

  • Neglecting spatial derivatives, the equation is rewritten as

  • If the system has evolved into attractor regime,

  • We choose the uniform scalar slicing ,

  • The conservation of curvature perturbation is shown

  • without specifying gravity theory.


G ≠ 0

  • The lowest order equation in gradient expansion is

  • There is asecond derivative of Ψ (= derivative of K),

  • → we cannot show the conservation W/O Einstein equation.

  • Once we invoke Einstein gravity, we can replace K,τ with K.

Again, in the attractor stage, we can show the conservation of

curvature perturbation on the uniform scalar field slice.


Summary
summary

  • Using the gradient expansion approach, we have studied

    the evolution of curvature perturbation on superhorizon scales

    in the case of single scalar field inflation.

  • In the cases of canonical and k-essential scalar field (G = 0),

  • we have shown the conservation of curvature perturbation

  • without specifying gravity theory using scalar field equation.

  • The condition for the conservation is whether the system

  • has evolved into a attractor regime.


Summary 2
summary 2

  • In the case of galileon field, the conservation has not been

    shown without invoking gravity theory because there appear

    a second derivative of Ψ in the scalar field equation.

  • Once we have usedthe Einstein equation, we can rewrite the

    second derivative by first derivative and we can show the

    conservation of curvature perturbation in the attractor stage.


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