dynamics of cosmological relaxation after reheating...conclusion 1. high reheating temperature is...
TRANSCRIPT
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The 3rd IBS-MultiDark-IPPP WorkshopNovember 24 2016
Dynamics of cosmological relaxation after reheating
Hyungjin Kim
KAIST & IBS CTPU
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[Graham, Kaplan, Rajendran 15]
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[Graham, Kaplan, Rajendran 15]
m2h(�0) ⇠ �(90GeV)2
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[Graham, Kaplan, Rajendran 15]
• Relaxion dependent Higgs mass
• Higgs vev dependent Back-reaction potential
• Inflationary Hubble friction
Necessary ingredients for relaxion are
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Whole scanning process take place during inflation
What happens after the reheating ?
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Two possible scenarios
• Reheating temperature higher than electroweak scale
• Reheating temperature lower than electroweak scale
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Two possible scenarios
• Reheating temperature higher than electroweak scale
• Reheating temperature lower than electroweak scale
• thermal correction is small
• barrier is still there
• relaxion does not evolve
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Two possible scenarios
• Reheating temperature higher than electroweak scale
• Reheating temperature lower than electroweak scale
• thermal correction is small
• barrier is still there
• relaxion does not evolve
• thermal correction is large
• barrier disappears
• relaxion evolves!
• gauge symmetry is restored
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(positive)
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(positive)
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To preserve successful selection of electroweak scale
we need small enough field velocity
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To preserve successful selection of electroweak scale,
we require
otherwise, the selection of electroweak scale is easily ruined
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Dynamically selected EW scale is not stable against high reheating temperature
Alternative possibility?
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A possibility:
A new frictional force from Abelian gauge boson
[Choi, HK, Toyokazu; Work in progress]
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A possibility:
A new frictional force from Abelian gauge boson
[Choi, HK, Toyokazu; Work in progress]
• Friction from Hubble
• Friction from gauge field production
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A possibility:
A new frictional force from Abelian gauge boson
[Choi, HK, Toyokazu; Work in progress]
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Anomalous coupling
time-dependent coupling breaks conformal invariance
and develops instability of gauge boson
[Anber & Sorbo, 09]
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Dispersion relation
propagatingmode
tachyonicmode
for
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Dispersion relation
and exponentially grows in time
tachyonic mode exists for
&
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Background evolution of scalar field develops instability
and exponentially produces gauge bosons
Produce X
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Background evolution of scalar field develops instability
and exponentially produces gauge bosons
How does X field modify the field velocity of relaxion ?
Produce X
modifies
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Evolution of scalar field
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force
Evolution of scalar field
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velocity-dependent
friction
Evolution of scalar field
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“gauge”friction
Evolution of scalar field
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Evolution of scalar field
terminal velocity is determined as
�̇ = ⇠FXH
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Evolution of scalar field
terminal velocity is determined as
�̇ = ⇠FXH
decreasing function in time!
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When does it stop?
barrier is formed at T ⇠ Tc
�̇2 ⇤4b ?
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When does it stop?
barrier is formed at T ⇠ Tc
�̇2 ⇤4b ?
Yesrelaxion stops at Tc
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When does it stop?
barrier is formed at T ⇠ Tc
�̇2 ⇤4b ?
Yesrelaxion stops at Tc
No
relaxion stops at Tb
�̇2(Tb) ⇠ ⇤4b* Tb is when
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When does it stop?
relaxion will stop at
Ts = min(Tc, Tb)
barrier is formed at T ⇠ Tc
�̇2 ⇤4b ?
Yesrelaxion stops at Tc
No
relaxion stops at Tb
�̇2(Tb) ⇠ ⇤4b* Tb is when
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To preserve successful selection of electroweak scale
��(ts)
(
�V
�V ⇤2v2
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To preserve successful selection of electroweak scale
��(ts)
(
�V
�V T 4s ⇤2v2
To prevent overproduction of dark gauge boson
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106 107 108 109 1010 1011 1012102
104
106
108
1010
1012
1014
1016
1018
10-2
10-4
10-6
10-8
10-10
10-12
10-14
10-16
10-18
Gauge field overproduction
�Ne↵ �
0.3
✓h� = 10�20
✓h� = 10�15
✓h� = 10�10
[Choi, HK, Toyokazu; Work in progress]
Preliminary
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106 107 108 109 1010 1011 1012102
104
106
108
1010
1012
1014
1016
1018
100
10-2
10-4
10-6
10-8
10-10
10-12
10-14
10-16
Gauge field overproduction
Fifth force
SN1978A
✓h� = 10�20
✓h� = 10�15
✓h� = 10�10
�Ne↵ �
0.3
Preliminary
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106 107 108 109 1010 1011 1012102
104
106
108
1010
1012
1014
1016
1018
102
100
10-2
10-4
10-6
10-8
10-10
10-12
10-14
Fifth force
Gauge field overproduction
SN1978A
LHC
Globular Cluster
�Ne↵ �
0.3
✓h� = 10�5
✓h� = 10�15
✓h� = 10�10
[Choi & Im 16][Flacke et. al. 16]
regarding constraints on relaxion scenario
Preliminary
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Conclusion
1. High reheating temperature is dangerous for cosmological relaxation
2. If relaxion has anomalous coupling to Abelian gauge boson,
it transfer its kinetic energy into gauge bosons
3. Field velocity approaches to terminal velocity,
4. The relaxion can be re-captured by back-reaction potential at EWPT
under reasonable choice of parameters