Gravitational waves from first-order phase transitions: Towards - PowerPoint PPT Presentation

Gravitational waves from first-order phase transitions: Towards understanding ultra-supercooled transitions Ryusuke Jinno (DESY) Based on 1905.00899 with Hyeonseok Seong (IBS & KAIST), Masahiro Takimoto (Weizmann), Choong Min Um (KAIST) 2019/5/11 @ NHWG 25th regular meeting 01 / 19

Introduction

ERA OF GRAVITATIONAL WAVES Detection of GWs from BH & NS binaries → GW astronomy has started - Black hole binary 36M ⊙ + 29M ⊙ → 62M ⊙ - Frequency ~ 35 to 250 Hz - Significance > 5.1 σ [LIGO] Ryusuke Jinno, 02 / 19 1905.00899 "GWs from first-order phase transitions: Ultra-supercooled transitions and the fate of relativistic shocks"

ERA OF GRAVITATIONAL WAVES Next will be GW cosmology with space interferometers 重力波天文学のロードマップ 地上望遠鏡 宇宙望遠鏡 Ground Space より遠くを観測 (10Hz-1kHz) 低周波数帯の観測 (1Hz 以下 ) LIGO TAMA CLIO VIRGO GEO Enhanced LIGO LPF 2010 Advanced Advanced LPF KAGRA Virgo LIGO DPF 2015 LISA KAGRA Ａｄ . ＬＩＧＯ Pre- ET DECIGO LISA 2020 & Taiji, TianQin 0.1mHz-10mHz DECIGO 確実な重力波源 ~10 event/yr のイベントレート BBO 2025 0.1Hz 帯 宇宙論的な重力波 DECIGO 原始重力波シンポ 日本物理学会 年秋季大会 年 月 日 佐賀大学 From Ando-san’s talk @ JPS meeting 2014 Ryusuke Jinno, 02 / 19 1905.00899 "GWs from first-order phase transitions: Ultra-supercooled transitions and the fate of relativistic shocks"

ERA OF GRAVITATIONAL WAVES Sensitivity curves for current & future experiments Pulsar timing arrays Space Ground -8 2 0.01-1Hz 10 Hz 10 Hz Taiji, TianQin SOGRO [http://rhcole.com/apps/GWplotter/] Ryusuke Jinno, 02 / 19 1905.00899 "GWs from first-order phase transitions: Ultra-supercooled transitions and the fate of relativistic shocks"

SOURCES FOR COSMOLOGICAL GWS Inflationary quantum fluctuations (“primordial GWs”) Preheating (particle production just after inflation) Topological defects : e.g. cosmic strings, domain walls First-order phase transition often occurs when a symmetry breaks: - PQ sym. breaking - Electroweak sym. breaking (w/ extension) - Breaking of GUT group ... - B-L breaking - Strong dynamics Ryusuke Jinno, 03 / 19 1905.00899 "GWs from first-order phase transitions: Ultra-supercooled transitions and the fate of relativistic shocks"

SOURCES FOR COSMOLOGICAL GWS Inflationary quantum fluctuations (“primordial GWs”) Preheating (particle production just after inflation) Topological defects : e.g. cosmic strings, domain walls First-order phase transition often occurs when a symmetry breaks: - PQ sym. breaking - Electroweak sym. breaking (w/ extension) - Breaking of GUT group ... - B-L breaking - Strong dynamics Ryusuke Jinno, 03 / 19 1905.00899 "GWs from first-order phase transitions: Ultra-supercooled transitions and the fate of relativistic shocks"

ROUGH SKETCH OF PHASE TRANSITION & GW PRODUCTION How first-order phase transition produces GWs Field space Position space false vacuum true vacuum true (“nucleation”) false true released energy V true x 3 Φ Quantum tunneling Bubble formation & GW production Ryusuke Jinno, 04 / 19 1905.00899 "GWs from first-order phase transitions: Ultra-supercooled transitions and the fate of relativistic shocks"

ROUGH SKETCH OF PHASE TRANSITION & GW PRODUCTION How first-order phase transition produces GWs Field space Position space GWs ⇤ h ij ∼ T ij false vacuum true vacuum true Bubbles released true source GWs energy V true Φ Quantum tunneling Bubble formation & GW production Ryusuke Jinno, 04 / 19 1905.00899 "GWs from first-order phase transitions: Ultra-supercooled transitions and the fate of relativistic shocks"

TALK PLAN 0. Introduction ✔ 1. GW production in ultra-supercooled transitions 2. Effective theory of shock propagation 3. Summary Ryusuke Jinno, / 19 1905.00899 "GWs from first-order phase transitions: Ultra-supercooled transitions and the fate of relativistic shocks"

zero-temperature eff. potential BEHAVIOR OF BUBBLES m ρ released Transition in vacuum cosmological scale - Bubbles nucleate with "particle scale" m − 1 ( : typical mass scale of the potential, say, TeV) m false true - Bubble surfaces = "walls" (= where the scalar field value changes) - As bubbles expand to "cosmological scale", ∼ ∼ the released energy accumulates on the wall φ - Resulting factor can be huge: γ ∼ ∼ r or more at the time of collision ∼ 10 10 γ m − 1 m − 1 γ − 1 Ryusuke Jinno, 05 / 19 1905.00899 "GWs from first-order phase transitions: Ultra-supercooled transitions and the fate of relativistic shocks"

thermal potential BEHAVIOR OF BUBBLES ρ released Transition in thermal environment cosmological scale - Two main players : scalar field and plasma false pressure - Walls want to expand (“pressure”) wall Controlled by α ≡ ρ released scalar+plasma dynamics ρ plasma friction true - Walls are pushed back by plasma (“friction”) φ Controlled by coupling btwn. scalar and plasma η - Let's see how bubbles behave for different α ∼ ∼ r (with fixed ) η m − 1 m − 1 Ryusuke Jinno, 06 / 19 1905.00899 "GWs from first-order phase transitions: Ultra-supercooled transitions and the fate of relativistic shocks"

BUBBLE EXPANSION IN α ≡ ρ released THERMAL TRANSITION ρ plasma [ Espinosa, Konstandin, No, Servant ’10 ] Small T / T ∞ Temperature α ( . O (0 . 1)) “deflagration” 1.2 1.0 0.8 0.6 wall position 1.0 r / t 0.0 0.2 0.4 0.6 0.8 Fluid outward velocity v fluid 0.5 0.4 0.3 0.2 0.1 wall position 1.0 r / t 0.0 0.2 0.4 0.6 0.8 Ryusuke Jinno, 07 / 19 1905.00899 "GWs from first-order phase transitions: Ultra-supercooled transitions and the fate of relativistic shocks"

BUBBLE EXPANSION IN α ≡ ρ released THERMAL TRANSITION ρ plasma [ Espinosa, Konstandin, No, Servant ’10 ] Small but slightly increased α ( . O (0 . 1)) Temperature T / T ∞ 1.3 “detonation” 1.2 1.1 1.0 0.9 wall position 1.0 r / t 0.0 0.2 0.4 0.6 0.8 Fluid outward velocity v fluid 0.4 0.3 0.2 0.1 wall position 1.0 r / t 0.0 0.2 0.4 0.6 0.8 Ryusuke Jinno, 1905.00899 "GWs from first-order phase transitions: Ultra-supercooled transitions and the fate of relativistic shocks" 07 / 19

BUBBLE EXPANSION IN α ≡ ρ released THERMAL TRANSITION ρ plasma [ Espinosa, Konstandin, No, Servant ’10 ] Large Temperature α ( � 1) T / T ∞ wall position 5 “strong detonation” 4 3 2 1 r / t 0.0 0.2 0.4 0.6 0.8 1.0 Fluid outward velocity γ fluid 14 wall position 12 10 8 6 4 2 r / t 0.0 0.2 0.4 0.6 0.8 1.0 Ryusuke Jinno, 1905.00899 "GWs from first-order phase transitions: Ultra-supercooled transitions and the fate of relativistic shocks" 07 / 19

KNOWNS AND UNKNOWNS The system BEFORE bubble collisions is relatively known - Nucleation rate is calculable from the potential (note but : gauge-dependence is an issue when the scalar field is gauged) [ e.g. Chiang & Senaha '17 ] - Behavior of fluid (i.e. coarse-grained plasma) is calculable from ∂ µ T µ ν fluid = 0 with an energy-injection boundary condition at the wall position Less known is the system AFTER collisions - This is important to predict GWs = observable Ryusuke Jinno, 08 / 19 1905.00899 "GWs from first-order phase transitions: Ultra-supercooled transitions and the fate of relativistic shocks"

KNOWNS AND UNKNOWNS The system BEFORE bubble collisions is relatively known - Nucleation rate is calculable from the potential (note but : gauge-dependence is an issue when the scalar field is gauged) [ e.g. Chiang & Senaha '17 ] - Behavior of fluid (i.e. coarse-grained plasma) is calculable from ∂ µ T µ ν fluid = 0 with an energy-injection boundary condition at the wall position Less known is the system AFTER collisions - This is important to predict GWs = observable Ryusuke Jinno, 08 / 19 1905.00899 "GWs from first-order phase transitions: Ultra-supercooled transitions and the fate of relativistic shocks"

DYNAMICS AFTER COLLISION Bubbles nucleate & expand - Nucleation rate (per unit time & vol) Γ ( t ) ∝ e β t with 1 / β : some const. - Released energy is mainly carried by fluid motion [ Bodeker & Moore ’17 ] - Typically collide after expansion ∆ t ∼ 1 / β Ryusuke Jinno, 09 / 19 1905.00899 "GWs from first-order phase transitions: Ultra-supercooled transitions and the fate of relativistic shocks"

DYNAMICS AFTER COLLISION Bubbles nucleate & expand - Nucleation rate (per unit time & vol) Γ ( t ) ∝ e β t with 1 / β : some const. - Released energy is mainly carried by fluid motion [ Bodeker & Moore ’17 ] - Typically collide after expansion ∆ t ∼ 1 / β Ryusuke Jinno, 09 / 19 1905.00899 "GWs from first-order phase transitions: Ultra-supercooled transitions and the fate of relativistic shocks"