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Gravitational waves and cosmology. P. Binétruy APC, Paris. 6th Rencontres du Vietnam Hanoi, August 2006. At t = 400 000 yrs, the Universe becomes transparent: photons no longer interact with matter. Looking back to the primordial Universe. BIG BANG. Cosmological background

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gravitational waves and cosmology

Gravitational waves and cosmology

P. Binétruy

APC, Paris

6th Rencontres du Vietnam

Hanoi, August 2006

slide2

At t = 400 000 yrs, the Universe becomes transparent: photons no longer interact with matter

Looking back to the primordial Universe

BIG BANG

Cosmological background

T = 3 K = - 270 °C

WMAP satellite

slide3

And before?

?

gravitons and neutrinos

slide5

When do graviton decouple?

T5

Interaction rate

~ GN2 T5 ~ ----

MPl4

T2

Expansion rate

H ~ ----

(radiation dominated era)

MPl

T3

---- ~ ----

H

MPl3

Gravitons decouple at the Planck era : fossile radiation

slide6

But gravitons could be produced after the Planck era.

Gravitons of frequency f* produced at temperature T* are observed

at a redshifted frequency

1/6

f = 1.65 10-7 Hz --- ( ----- ) ( ---- )

1

T*

g*

1GeV

100

At production * =  H*-1 (or f* = H*/ )

Horizon length

Wavelength

slide7

LF band0.1 mHz - 1 Hz

Gravitational wave detection

VIRGO

slide8

d GW

1

GW = --- --------

, c = 3H0/(8GN)

c

d logf

for =1

slide9

Electroweak phase transition

If the transition is first order,

nucleation of true vacuum bubbles

inside the false vacuum

Collision of bubbles  production of gravitational waves

Pros and cons for a 1st order EW phase transition:

  • in the Standard Model, requires mh < 72 GeV (ruled out)
  • in the MSSM, requires a light stop (less and less probable)
  • possible to recover a strong 1st order transition by including 6 terms
  • in SM potential
  • needed to account for baryogenesis at the electroweak scale (out
  • of equilibrium dynamics)
slide10

Efalse vac

 = ---------

aT*4

h02 GW

radiation energy

at transition

Nicolis

gr-qc/0303084

f in mHz

turbulence

bubble collision

fturb/fcoll~ 0.65 ut/vb

slide11

Long wavelength GW produce a

redshift on the photons of the CMB

Wavelength outside the horizon at LSS

Wavelength inside the horizon today

slide14

Vacuum fluctuations : de Sitter inflation (constant vacuum energy)

h02GW =10-13(feq/f) 2(H/10-4MPl)2

h02GW =10-13 (H/10-4MPl)2

Fluctuations reenter horizon during matter era radiation era

slide15

More realistic inflation models : slowroll

nT

h02 GW ~ V f

nT = - (V’/V)2 MPl2 /8 = -T/7S

slide17

Cosmic strings

Presence of cusps enhances the production of gravitational waves

Damour-Vilenkin

log h

LIGO

stochastic GW

background

log 50 GN

Loops radiate at

z>1 (MD)

z>1 (RD)

z<1

slide18

How to measure a stochastic background?

Cross correlate

ground interferometers

Let LISA move around the Sun

slide19

2. Dark energy: in search of standard candles

  • Supernovae of type Ia

magnitude versus redshift

mB = 5 log(H0dL) + M - 5 log H0 + 25

  • Gamma ray bursts
  • Coalescence of black holes : the ultimate standard candle?
slide20

Gravitational dynamics

f ~ (G)1/2

R in m

f = 10-4 Hz

space interf.

109

f = 1Hz

ground interf.

f = 104 Hz

104

100

108

M/M

slide21

Gravitational dynamics

Schwarzchild radius

R = 2GM/c2

R in m

space interf.

109

ground interf.

black hole line

104

100

108

M/M

slide22

Gravitational dynamics

Supermassive BH mergers

R in m

space interf.

109

chirp line

coalesc. in 1 yr

ground interf.

black hole line

104

100

108

M/M

NS-NS coalescence

after B. Schutz

slide24

Inspiral phase

(m1 m2)3/5

Key parameter : chirp mass M =

(1+z)

(z)

(m1 + m2)1/5

slide25

Inspiral phase

(m1 m2)3/5

Key parameter : chirp mass M =

(1+z)

(z)

(m1 + m2)1/5

Amplitude of the gravitational wave:

frequency

f(t) = d/2dt

M(z)5/3 f(t)2/3

h(t) = F (angles) cos (t)

dL

Luminosity distance

slide26

Inspiral phase

(m1 m2)3/5

Key parameter : chirp mass M =

(1+z)

(z)

(m1 + m2)1/5

Amplitude of the gravitational wave:

M(z)5/3 f(t)2/3

h(t) = F (angles) cos (t)

dL

Luminosity distance

poorly known in the case of LISA

10 arcmin

1 Hz

~

SNR

fGW

slide27

z = 1 , m1 = 105 M, m1 = 6.105 M

(arcminutes)

5%

Holz & Hughes

dL/dL

slide28

Using the electromagnetic counterpart

Allows both a measure of the direction and of the redshift

0.5%

Holz and Hughes

dL/dL

But limited by weak gravitational lensing!

dL/dLlensing= 1-1/

slide29

Conclusions

  • LISA will provide complentary ways to identify the geometry
  • of the Universe.
  • regarding a stochastic background of primordial gravitational
  • waves, no detection in the standard inflation scenarios, but many
  • alternatives lead to possible signals within reach of advanced
  • ground interferometers or LISA.
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