Loading in 2 Seconds...

Nonlinear curvature perturbations in two-field hybrid inflation

Loading in 2 Seconds...

- By
**tamah** - Follow User

- 99 Views
- Uploaded on

Download Presentation
## PowerPoint Slideshow about ' Nonlinear curvature perturbations in two-field hybrid inflation' - tamah

**An Image/Link below is provided (as is) to download presentation**

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.

- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -

Presentation Transcript

### Nonlinear curvature perturbations in two-field hybrid inflation

5-9 March, 2008

-- dN in exactly soluble models --

Yukawa Institute (YITP)

Kyoto University

Misao Sasaki

kanreki = one cycle of

chinese zodiacal calendar

祝還暦

60 yrs =

12 animals

x 5 elements

chan-chanko

clothing

this (Andrei’s) year

Red signifies

a baby

mouse x earth

also, Red is a color

of happiness

reliability

productivity

A person is regarded as reborn on the 60th birthday

1. Success of Inflation

(slow-roll) inflation

Linde ’82, ...

explains the origin of cosmological perturbations.

....

finally observed by COBE & WMAP!

Inflation from string theory

KKLMMT ’03, ...

brane/DBI inflation, moduli inflation, ...

may lead to large non-Gaussianity.

−9 < fNLlocal < 111 (WMAP 5yr)

may be detected in the very near future

Why care about soluble models?

In this talk, I analyze full nonlinear curvature perturbations

in exactly soluble models of slow-roll inflation

Using dN formalism,

(dN··· e-folding number perturbation)

- We can explicitly see how and when curvature
- perturbations are generated.

- Non-Gaussianity can be explicitly evaluated.

We may deepen our understanding of

cosmological perturbations.

tatemae

(建前)

hon-ne

(本音)

Because it’s fun!

2. dN for curvature perturbations

Starobinsky ‘85, MS & Stewart ‘96, MS & Tanaka \'98,

Lyth, Malik & MS ‘04,....

Separate universe (gradient expansion) approach

Belinski et al. ’70, Tomita ’72, Salopek & Bond ’90, …

- each Hubble region evolves independently

- perturbations on superhorizon scales
- ≈ difference between different FLRW universes

- calculate dN for different FLRW universes

٠٠٠ curvature perturbation

on comoving slice

defined by an integral

=non-local quantity

→ gauge invariance

dN for ‘slowroll-type’ inflation

MS & Tanaka ’98, Lyth & Rodriguez ’05, ...

- In slowroll inflation, all decaying mode solutions of the
- (multi-component) scalar field f die out.

→ N=indep. of df/dt

where df =dfF (on flat slice) at horizon-crossing.

- The above formula is valid for any model in which
- N is only a function of f but not of df/dt.

(e.g., power-law inflation)

3. Exactly soluble slow-roll models

(a,b= 1,2,...,n)

Slow-roll equations of motion

e-folding number from the end of inflation

An exactly soluble class

If

for each a

(a= 1,2,...,n)

this is sufficient

(slowroll unnecessary)

Then

...

new field space

coordinates

··· na is conserved

solvability (n-1) constants of integration

- Nonlinear dN is

- Linear curvature perturbation is given by

where (q, na) and (dq, dna) are the values at horizon

crossing during inflation

curvature perturbation generated from adiabatic & “entropy” perturbations

perturbations orthogonal to dqa/dN

adiabatic perturbation

entropy perturbation during inflation

Polarski & Starobinsky ’94,

Mukhanov & Steinhardt ’97, MS & Tanaka ’98,...

entropy perturbation at the end of inflation

Bernardeau, Kofman & Uzan ‘04, Lyth ‘05, ...

f

inflation

4. Two (plus one)-field hybrid inflation∙ can be easily generalized to n fields

“n-brid inflation”

- slow-roll eom:

- transformation of variables:

and the universe is thermalized instantaneously.

realized by

Parametrize orbits by an angle at the end of inflation

This determines g in terms of f1 & f2 .

whereg=g(f1,f2)

- dN valid to full nonlinear order is simply given by

To be precise, one has to add a correction term to adjust

- the energy density difference at the end of inflation

where

(assuming instantaneous thermalization)

However, this correction is negligible

if

- comoving curvature perturbation spectrum

spectral index:

tensor/scalar:

- single-field case

No non-Gaussianity if dfis Gaussian

“true” entropy perturbation

linear entropy perturbation

contributes at 2nd order

practically any non-Gaussianity is possible

So, here is a birthday present for you, Andrei.

hope you like it...

5. Summary

- Exactly soluble models are useful in understanding
- generation of (nonlinear) curvature perturbations

- Curvature perturbation may be generated from both
- adiabatic and entropy perturbations during inflation

- In multi-field models, final amplitude of curvature
- perturbation depends crucially on how inflation ends.

- n-brid inflation looks like an almighty model!

(classically. negligible quantum corrections assumed)

Download Presentation

Connecting to Server..