- 100 Views
- Uploaded on
- Presentation posted in: General

Inflation : why and how ?

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 - - - - - - - - - - - - - - - - - - - - - - - - - -

Inflation: whyandhow?

Gert Jan Hoeve, December 2012

- Flatness
- |Ω-1|<1016 at nucleosythesis

- Homogeneity over parts of spacethat are presumablynotcausallycorrelated.

- Conventionaltheories of symmetrybreaking are insufficientfor the observedammount of baryons

d2a/dt2 >> 0

or equivalently,

-(dH/dt)/H2 >> 1

Between Planck time (10-43) andGUT decoupling (10-35)

Alan Guth, 1981

Picture: Wikipedia

- Ω is pushedtowards 1 duringinflation
- ‘Stretching’

- Abundant at high temperature
- Slow decay

- Cosmic Microwave Background radiationoriginated 500,000 yearsafter the BB.
- No causalcorrelationpossible

Picture: one minute astronomer

Inflationends at t0 = 10-35 s, we are at t1 = 1017 s

In radiationdominateduniverse |Ω-1|proportional to time

|Ωnow-1| ≤ 10-2 |ΩGUT-1|≤ 10-54

Recall|Ω-1|=|k|/(Ha)2

Duringinflation H=constant, so|Ω-1|proportional to 1/a2

Total expansion > ~ 1027

- Three conditions (Sakharov’sconditions)
- Baryon numberviolatinginteractions
- obvious

- C violationand CP violation
- Becauseany B-violatinginteractionwouldbemirroredby a complementaryinteraction

- Thermal non-equilibrium (or CPT violation)
- Otherwise the backwardsreactionwouldbeequilly strong

- Baryon numberviolatinginteractions

- Standard model:
sphalerons

- Differenceleptonnumber
andbaryonnumerconserved

- Example:
(u+u+d)+(c+c+s)+(t+t+b) e++μ++τ+

- B-violatingprocess must outratesymmetricprocess
- Both symmetries
must beviolated

- Phasetransitionbubbles
- Thermal energy gradient at bubbleedge
- Local breakdown of time symmetry

Scalar field V(φ) causesspontaneoussymmetrybreaking

First or second order phasetransition?

B. Clauwens , R. Jeanerot, D-term inflationafterspontaneoussymmetrybreaking

H. Bohringer

- False/real vacuum
- First order phasetransition
- Reheatingproblems

- d2φ/dt2 + 3H dφ/dt = -dV(φ)/dφ
- Friedman H2 = (1/2 dφ/dt+V(φ))/3 –k/a2
- Inflationdecays as slopeincreases
- H=(da/dt)/a

- 5th fundamental force
- Continueousdecayingscalar field
- Couldexplaininflationanddark energy at the same time!

- M. Trodden, Baryogenesisand the new cosmology, 2002

Cosmologicalinflation is a viable hypothesis, but in desperate need of a more solid foundation (and experimental confirmation) from the realm of particle physics.