Large extra dimensions Randall-Sundrum Supersymmetry Z - - PowerPoint PPT Presentation

송희성 선생님과 공동연구 Large extra dimensions Randall-Sundrum Supersymmetry Z’ Radion Graviton 𝞯’/𝞯 in LR-model (g-2) Spin correlation rotating black holes

송희성 선생님과 공동 연구 (1999-2001)

Higgs as Inflaton

박성찬 (연세대)

고 송희성 교수님 추모 심포지움 2017.4.13.

3

Cut-off scale of the SM

Cut-off scale of the SM

• In principle, we can ‘calculate’ everything E< 𝝡SM

with unlimited precision.

Cut-off scale of the SM

• In principle, we can ‘calculate’ everything E< 𝝡SM

with unlimited precision.

• 𝝡SM > TeV, LHC

Cut-off scale of the SM

• In principle, we can ‘calculate’ everything E< 𝝡SM

with unlimited precision.

• 𝝡SM > TeV, LHC
• 𝝡SM ~ Mplanck, in principle as the SM is

renormalizable

Cut-off scale of the SM

• In principle, we can ‘calculate’ everything E< 𝝡SM

with unlimited precision.

• 𝝡SM > TeV, LHC
• 𝝡SM ~ Mplanck, in principle as the SM is

renormalizable

• We may extrapolate all the way up to the Planck

energy and see what would happen there.

Higgs + Gravity

V (H) = λ

• |H|2 − v2/2

2

S = Z d4x√g M 2

P +ξ|H|2

2 R + |DH|2 − V (H) + LSM

• dim=4

dim>4 + X

n=1

O4+n M n

Planck

Higgs=R2

Higgs=R2

S = Z d4x√g

• (1 + ξφ2)R + (∂φ)2 − λφ4

Higgs=R2

S = Z d4x√g

• (1 + ξφ2)R + (∂φ)2 − λφ4

**During inflation kinetic energy is not important so that φ can be regarded as an auxiliary field.

Higgs=R2

S = Z d4x√g

• (1 + ξφ2)R + (∂φ)2 − λφ4

**During inflation kinetic energy is not important so that φ can be regarded as an auxiliary field.

Higgs=R2

S = Z d4x√g

• (1 + ξφ2)R + (∂φ)2 − λφ4

**During inflation kinetic energy is not important so that φ can be regarded as an auxiliary field.

δφ : 2ξφR − 4λφ3 = 0

Higgs=R2

S = Z d4x√g

• (1 + ξφ2)R + (∂φ)2 − λφ4

**During inflation kinetic energy is not important so that φ can be regarded as an auxiliary field.

δφ : 2ξφR − 4λφ3 = 0

φ2 = ξ 2λR

• >

Higgs=R2

S = Z d4x√g

• (1 + ξφ2)R + (∂φ)2 − λφ4

**During inflation kinetic energy is not important so that φ can be regarded as an auxiliary field.

δφ : 2ξφR − 4λφ3 = 0

φ2 = ξ 2λR

• >

Higgs=R2

S = Z d4x√g

• (1 + ξφ2)R + (∂φ)2 − λφ4

**During inflation kinetic energy is not important so that φ can be regarded as an auxiliary field.

δφ : 2ξφR − 4λφ3 = 0

φ2 = ξ 2λR

• >

S = Z d4x√g ✓ R + ξ2 4λR2 + · · · ◆

Higgs=R2

S = Z d4x√g

• (1 + ξφ2)R + (∂φ)2 − λφ4

**During inflation kinetic energy is not important so that φ can be regarded as an auxiliary field.

δφ : 2ξφR − 4λφ3 = 0

φ2 = ξ 2λR

• >

S = Z d4x√g ✓ R + ξ2 4λR2 + · · · ◆

Starobinski (R2) inflation

α = ξ2 4λ

Higgs=R2

S = Z d4x√g

• (1 + ξφ2)R + (∂φ)2 − λφ4

**During inflation kinetic energy is not important so that φ can be regarded as an auxiliary field.

δφ : 2ξφR − 4λφ3 = 0

φ2 = ξ 2λR

• >

S = Z d4x√g ✓ R + ξ2 4λR2 + · · · ◆

Starobinski (R2) inflation

α = ξ2 4λ

The Higgs potential in Einstein frame

The Higgs potential in Einstein frame

inflation here

The Higgs potential in Einstein frame

inflation here

The Higgs potential in Einstein frame

inflation here

EWSB here

Higgs inflation provides very good fit to the data!

Planck [Astron.Astrophys. 594 (2016)]

RG running of lambda

self int. gauge int.

This dominates over other interactions.

MC mass vs pole mass

2-loop effective coupling

criticality

Hamada, Kawai, Oda, SCP [PRL 2014, PRD2015]

• S. Moch, et al.,MITP report

[1405.4781]

Mt & MH from Higgs inflation

H i g g s I n f l a t i

• n

Hamada, Kawai, Oda, SCP [PRL(2014)] Hamada, Kawai, Oda, SCP, [PRD(2015)]

check with full EWPT & Gfitter

• S. Heinemeyer, R. Kogler, SCP in progress

Potential Synergy

Cosmological observation

especially primordial gravitational wave

=

Precision particle physics experiments

e.g. top quark mass