Stochastic background of gravitational waves from cosmological sources · 2014-07-29 · Stochastic...
Transcript of Stochastic background of gravitational waves from cosmological sources · 2014-07-29 · Stochastic...
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Stochastic background of gravitational waves from cosmological sources
Chiara Caprini
IPhT CEA-Saclay
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OUTLINE
• overview of GW from the early universe: basic properties
• upper bounds and sensitivities to GW stochastic backgrounds
• examples of sources operating in the early universe:
- inflation - particle production during inflation- preheating- cosmic strings- scalar field self-ordering- first order phase transitions in the early universe (EWPT, QCDPT)
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• particles that decouple at temperature carry direct information about the universe at that temperature
• the weakest the interaction, the earlier in the history of the universe the particles decouple
Tdec
�(T )H(T )
< 1rate of the interaction maintaining thermal
equilibrium rate of expansion of the universe
Primordial GW: “fossil radiation”
• they propagate freely after decoupling, without interaction
• as the universe expands, particles can get out of thermal equilibrium
� = n � v
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a few such decoupling events in the universe
history
GW: unique probe of the very early universe
inflation
radiation
matterdark
energy
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photons decouple: CMB
Tdec = 0.3 eV
• confirm big bang theory
• temperature fluctuations: seeds for structure formation
• informations on the physics generating them (inflation)
• ...
• informations on the content of the universe, the curvature
GW: unique probe of the very early universe
T0 ' 2 · 10�4 eVtoday :
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neutrinos decouple: background
Tdec = 1MeV
⌫
Tdec = 0.3 eV
• indirect evidence: CMB, structure formation, BBN
• masses, species...
photons decouple: CMB
GW: unique probe of the very early universe
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GW: unique probe of the very early universe
for gravitons in thermal equilibrium, the decoupling temperature would be Tdec = 1019 GeV
Tdec = 1MeV
Tdec = 0.3 eV
neutrinos decouple: background⌫
photons decouple: CMB
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GW: unique probe of the very early universe
detection of the GW “fossil radiation”: big step forward in our knowledge of the very early universe
because of the weakness of the gravitational interaction the universe is transparent to
primordial GW
GW from any generation process in the early universe carry direct information on
the process itself
GW source in the early universe ?
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GW from cosmological sources
Gµ� = 8�G Tµ�
source: tensor anisotropic stress
tensor perturbations of FRW metric: (hii = hi
j|j = 0)
ds2 = �dt2 + a2(t)[(�ij + hij)dxidxj ]
• fluid :
• electromagnetic field :
• scalar field :
hij + 3H hij + k2 hij = 16⇡G⇧ij
⇧ij
⇧ij ⇠ �2(⇢+ p) vivj
⇧ij ⇠(E2 +B2)
3� EiEj �BiBj
⇧ij ⇠ @i�@j�
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inflation: phase of accelerated expansion of the background
possibility of particle creation
a00
a= a2H2 > 0
GW from cosmological sources
source: amplification of vacuum fluctuations during inflation
v±(t) = MPl a(t)h±(t)
v00±(t) + (k2 � a2H2)v±(t) = 0
✓ canonically normalised free field✓ quantisation ✓ homogeneous wave equation✓ harmonic oscillator with time dependent frequency✓ quantum field : zero point fluctuations
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GW from cosmological sources
k � aH k ⌧ aH
v00±(t) + (k2 � a2H2)v±(t) = 0
free field in vacuumzero occupation number
!2(t) = k2
sub - hubble modes
nk = 0
super - hubble modes
!2(t) = �a2H2
super - horizon modes have occupation number very large
nk � 1
source: a spectrum of gravitons has been generated by the fast expansion of the background and the stretching of the modes outside the horizon
source: amplification of vacuum fluctuations during inflation
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stochastic background of GW
- causal source: many independent horizon volumes visible today
- inflation: intrinsic, quantum fluctuations that become classical (stochastic) outside the horizon
⇥hij(k)h⇤ij(q)⇤ = (2⇥)3�(k� q)|h(k)|2
statistical homogeneity and isotropy
power spectrum
• sources from the early universe: stochastic background of GW, statistically homogenous, isotropic and Gaussian
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GW energy density:
frequency today (redshifted by expansion)
�GW =⇥GW
⇥c=
hhij hiji32�G ⇥c
=Z
df
f
d�GW
d ln f
f =k
2�
a(t)a0
stochastic background of GW
⇥hij(k)h⇤ij(q)⇤ = (2⇥)3�(k� q)|h(k)|2
statistical homogeneity and isotropy
power spectrum
• sources from the early universe: stochastic background of GW, statistically homogenous, isotropic and Gaussian
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causal (not inflation) source of GW cannot operate beyond the cosmological horizon:
Characteristic frequency for causal sources
k⇤ H⇤
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temperature (energy density) of the universe at the source time
standard thermal history
characteristic frequency
today
H =a
a
causal (not inflation) source of GW cannot operate beyond the cosmological horizon:
k⇤ H⇤
fc =k⇤2⇡
a⇤a0
1.6 · 10�4 HzT⇤
1TeV
a =T0
T
Characteristic frequency for causal sources
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PTAeLISA
ET
10-9 10-7 10-5 0.001 0.1 10 100010-13
10-11
10-9
10-7
10-5
0.0011 102 104 106 108 1010
f HHzL
h2WGW
T HGeVLCharacteristic frequency for causal sources
adv LIGO
EWPTQCDPT
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PTAeLISA
adv LIGO
ET
Characteristic frequency for causal sources
10-9 10-7 10-5 0.001 0.1 10 100010-13
10-11
10-9
10-7
10-5
0.0011 102 104 106 108 1010
f HHzL
h2WGW
T HGeVL
QCDPT
physics beyond the standard model
EWPT
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InflationCosmological dark age (reheating, baryogenesis,
phase transitions...)BBN
CMBGW GW
light elements
QCDEWSUSYEPlanck MeV eV
�hij
eLISALIGO Pulsars
1016GeV
(BICEP2)
CMB
anisotropies
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• PPTA 2013
• LIGO science run 2005-2007
• Nucleosynthesis and CMB: measure of the relativistic energy density in the universe
• COBE, WMAP, Planck measured TEMPERATURE fluctuations in CMB
h2�GW < 7 · 10�11
✓H0
f
◆2
10�18 Hz < f < 10�16 Hz
Shannon et al 1310.4569
41 Hz < f < 169 Hz Abbott et al, 0910.5772
h2�GW < 6.9 · 10�6h2�GW . 7.8 · 10�6
h2�GW . 6.9 · 10�6
f > 10�10 Hz f > 10�16 Hz Smith et al, astro-ph/0603144
h2⌦GW < 1.3 · 10�9 f ' 2.8 nHz
Limits on a stochastic background
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Limits on a stochastic background
before BICEP2
COBE WMAP Planck
BBNCMBLIGO
PTA
10-18 10-14 10-10 10-6 0.01 10010-1510-1310-1110-910-710-5
0.00110-8 10-5 10-2 1 102 104 106 108 1010
f HHzL
h2WGW
T HGeVL
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COBE WMAP Planck
BBNCMBLIGO
PTA
(maybe) detection of GW from inflation by BICEP2 : POLARISATION
10-18 10-14 10-10 10-6 0.01 10010-1510-1310-1110-910-710-5
0.00110-8 10-5 10-2 1 102 104 106 108 1010
f HHzL
h2WGW
T HGeVLLimits on a stochastic background
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• temperature : limit by COBE, WMAP, Planck
distortion of an homogeneous photon patch by GW :
imprint quadrupole anisotropy in the photon
distribution
GW influence CMB photons and leave an imprint in CMB anisotropies
• polarisation: BB spectrum measured by BICEP2 generated at photon decoupling time, from Thomson scattering of electrons by a quadrupole temperature anisotropy in the photons
�T
T= �
Z t0
tdec
hij ninjdt
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GW influence CMB photons and leave an imprint in CMB anisotropies
if the incident radiation is not isotropic, the scattered light at the end of decoupling (CMB)
is polarised
• polarisation: BB spectrum measured by BICEP2 generated at photon decoupling time, from Thomson scattering of electrons by a quadrupole temperature anisotropy in the photons
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GW influence CMB photons and leave an imprint in CMB anisotropies
polarisation patterns (independent on the reference frame)
generated by scalar and tensor
perturbations
generated only by tensor
perturbations (or foregrounds)
• polarisation: BB spectrum measured by BICEP2 generated at photon decoupling time, from Thomson scattering of electrons by a quadrupole temperature anisotropy in the photons
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B polarisation power spectra from BICEP last release
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GW background from inflation
measured by CMB
temperature
measured by CMB B
polarisation
from the measurement of T/S one can infer the energy scale of inflation
V 1/4 ' 2.25 · 1016 GeV⇣ r
0.2
⌘1/4
high scale inflation
amplitude of scalar perturbations
power spectrum/ 1
✏
H2
MP=
1
✏
V
M4P
amplitude of tensor perturbations power
spectrum/ H2
MP=
V
M4P
S
T
inflation amplifies both vacuum fluctuations of graviton (tensor mode) and of the scalar field driving inflation (scalar mode)
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GW background from inflation
smooth transition no particle
creation
abrupt transition particle creation
H0 < k < Heq
Heq < k < Hinf
k > Hinf
d �GW
d ln k⇠ 10�5
✓Hinf
mPl
◆2 ✓k
keq
◆nT
enter the horizon in the MD era
Grishchuk 1974, Starobinsky 1979, Abbott and Harari 1986, ...
V 1/4 ' 2.26 · 1016GeV
PTAeLISA ET
LIGOBBN
10-19 10-14 10-9 10-4 10 10610-18
10-15
10-12
10-9
10-6
f HHzL
h2WGW
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BUT... there are other possible sources of GW in the early universe promising for detection with
future interferometers or PTA
hij + 3H hij + k2 hij = 16⇡G⇧ij
mechanisms that produce a non-zero tensor anisotropic stress
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• fluid stiffer than radiation after inflation
• scalar field self-ordering
• primordial black holes
• non-perturbative decay of SUSY flat directions
Possible GW sources in the early universe
• inflation
• preheating after inflation
• phase transitions at the end or during inflation
• particle production during inflation
• unstable domain walls
• ...
• first order phase transitions
• cosmic (super)strings
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GW background from particle production during inflation• production of particles in the time dependent background due to the evolution of
the inflaton field
• observable signal : gauge fields coupled to pseudoscalar inflaton in linear inflationary potential
Cook and Sorbo 2012 Barnaby et al 2012
1e-16
1e-14
1e-12
1e-10
1e-08
1e-12 1e-10 1e-08 1e-06 0.0001 0.01 1 100 10000
!G
W h
2
f / Hz
NCMB = 60
(p=1) !LISA
!
ET
!
AdvLIGO
"CMB = 2.66
"CMB = 2.33
" = 0
1
4
�
fFµ⌫ Fµ⌫
⇠CMB
amplitude of the coupling
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• reheating: the energy density driving inflation is converted in radiation and matter
• preheating: possible first stage of this conversion, the inflaton decays in an explosive and highly inhomogeneous way
after hybrid inflation
after chaotic inflation
Kofman et al 1994, Khlebnikov and Tkachev 1997, ..., Dufaux et al 2009
f⇤ �4 · 1010 Hz
R⇤ �1/4p
size of the inhomogeneitiesR⇤
GW background from preheating
!
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GW background from cosmic strings
Kibble 1976, Vilenkin 1985, Damour and Vilekin 2000, Sarangi and Tye 2002 ..., Binetruy et al 2012
• one dimensional topological defects formed during symmetry breaking phase transitions or in the context of string theory at the end of brane inflation
• form a cosmological network which reach a scaling regime: it looks statistically the same at any time, the only relevant scale is the Hubble length
• decay by GW emission : long strings intercommute and form smaller loops which oscillate relativistically and emit GW
new loops from the long strings continually replace the loops that
disappearcontinuous GW production
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GW background from cosmic strings
• spectral shape extended in frequency because of continuous production
• parameters: tension, reconnection probability (loop size: probably solved)
ELISAPulsars
LIGO
aLIGO
GΜ"10#8
GΜ"10#11
GΜ"10#13
GΜ"10#12
GΜ"10#13
GΜ"10#17
10#12 10#9 10#6 0.001 1 100010#12
10#10
10#8
10#6
10#4
f !Hz"
h2$gw
p"10#3
p"1
Binetruy et al 2012
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GW background from scalar field self-ordering
• spectral shape extended in frequency because of continuous production
Fenu et al 2009
• after the spontaneous breaking of a global symmetry, N component scalar field gets different vev in different causal patches
• horizon grows, the field re-orders but anisotropic stress is present at the boundaries and sources GW
!
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• collisions of bubble walls • magnetohydrodynamic turbulence in the
primordial fluid
potential barrier separates true and false vacua
quantum tunneling across the barrier : nucleation of bubbles of true vacuum
source: tensor anisotropic stress
GW background from first order phase transitions
⇧ij
universe expands and temperature decreases : PTs , if first order lead to GW
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10!8 10!6 10!4 0.01 110!1810!1610!1410!1210!1010!810!6
f !Hz"
h2"GW!f"
SM # dimension six operator, Η%0.2
Huber and Konstandin 2008
increasing strength
eLISA
GW background from first order phase transitions : EWPT
Binetruy et al 2012
eLISA frequency bandT⇤ ' 100GeV
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10!5 10!4 0.001 0.01 0.1 110!11
10!10
10!9
10!8
10!7
f !Hz"
h2"GW!f"
Holographic Phase TransitionRandall and Servant 2007
Konstandin et al 2010
T⇤ ' 104 GeV
T⇤ ' 100 GeV
eLISA
GW background from first order phase transitions : EWPT
Binetruy et al 2012
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T⇤ = 100MeV
10−10 10−8 10−6 10−4 10−210−15
10−10
10−5
100
f [Hz]
h2 1(f)
Current NANOGrav sensitivity
PTA 2020
LISA
QCDPT : if lepton asymmetry is large Schwarz and Stuke 2009
GW background from first order phase transitions : QCDPT
CC et al 2010
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Conclusions
• we have little information about the physics and the processes operating in the very early universe
• but it is in principle possible to generate a stochastic background of GW detectable by them : preheating, cosmic strings, PTs...
• GW are a powerful mean to learn about the early universe and high energy physics: detection is extremely difficult but great payoff
• due to their small interaction rate, GW can in principle provide us with this information
• the frequency of GW maps the temperature/energy scale in the early universe
• GW by inflation at the energy scale indicated by the recent BICEP2 result are not visible with the next generation interferometers or by PTA