/18. Toshinori Matsui KIAS. Probing the first order electroweak phase transi5on by measuring gravita5onal waves in scalar extension models

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1 Probing the first order electroweak phase transi5on by measuring gravita5onal waves in scalar extension models Toshinori Matsui KIAS Collaborators: Katsuya Hashino 1, Mitsuru Kakizaki 1, Shinya Kanemura 1, Pyungwon Ko 2 1 University of TOYAMA, 2 KIAS M.Kakizaki, S.Kanemura, T.Matsui, Phys. Rev. D 92, no. 11, (2015), K.Hashino, M.Kakizaki, S.Kanemura, T.Matsui, Phys. Rev. D 94, no. 1, (2016), K.Hashino, M.Kakizaki, S.Kanemura, T.Matsui, P.Ko, arxiv: /18

2 Probing the first order electroweak phase transi5on by measuring gravita5onal waves in scalar extension models Contents Motivation: Physics behind the EWSB Electroweak Baryogenesis - 1 st order phase transition (1stOPT) hhh coupling & GWs GWs from 1stOPT Models of 1stOPT ( O(N) model & Higgs singlet model ) - Detectability at colliders and GW interferometers 1 /18

3 Probing the first order electroweak phase transi5on by measuring gravita5onal waves in scalar extension models Contents Motivation: Physics behind the EWSB Electroweak Baryogenesis - 1 st order phase transition (1stOPT) hhh coupling & GWs GWs from 1stOPT Models of 1stOPT ( O(N) model & Higgs singlet model ) - Detectability at colliders and GW interferometers 1 /18

4 Motivation - Physics behind EWSB Physics behind EWSB Discovery of the Higgs boson Mass genera[on mechanism is confirmed The Standard Model (SM) as the effec[ve theory is established Shape of the Higgs poten[al SM have minimal Higgs poten[al no principle Higgs poten[al The nature of EW symmetry breaking is not yet understood because Higgs self-couplings have not been measured BSM phenomena might be descried by extended Higgs sector Exploring the structure of the Higgs sector is important to understand physics behind EWSB. 2 /18

5 Motivation - EWBG Electroweak Baryogenesis Importance to understand the Higgs poten[al Observed Baryon number: Sakharov s 3 condi[ons 1. #B viola[on, 2. CP viola[on, 3. Departure from equilibrium V eff φ, T T T c T T c T T c Strongly 1 st order PT φ c φ SM cannot sa[sfy these condi[ons (m h =125GeV). 3 /18

6 Motivation - hhh 1stOPT & triple Higgs boson coupling 1stOPT is realized by models with extended Higgs sector. EWBG can be tested at future colliders HDM as an example of 500 the extended Higgs sector 400 The scenario of EWBG require Δλ hhh /λ hhh >O(10)%. m GeV Λ hhh O N Λ hhh SM φ c T c 1.0 m h 125 GeV m m H m A m H ± sin Β Α tanβ 1 Excluded by vacuum stability bound M GeV Kanemura, Okada, Senaha, PLB606 (2005) /18

7 Motivation - hhh 1stOPT & triple Higgs boson coupling 1stOPT is realized by models with extended Higgs sector. EWBG can be tested at future colliders. 2HDM The scenario of EWBG require Δλ hhh /λ hhh >O(10)%. 600 as an example of 500 the extended Higgs sector 400 Λ hhh O N Λ hhh SM 500 ILC1000-up (500/1000GeV, k -1 ) 200 Δλ hhh /λ hhh ~10% (ee ννhh) [K.Fujii et al., arxiv: ] m GeV 100 Δλ hhh /λ hhh >O(10)% 50 is testable at ILC (~10%@ s=1tev)! φ c T c 1.0 m h 125 GeV m m H m A m H ± sin Β Α tanβ 1 Excluded by vacuum stability bound M GeV Kanemura, Okada, Senaha, PLB606 (2005) /18

8 Motivation - GWs Gravita[onal waves Probing the Higgs poten[al by GW observa[ons LIGO have detected GWs directly. GW LIGO Scien[fic and Virgo Collabora[ons, Phys. Rev. Lew. 116, no. 6, (2016) GW LIGO Scien[fic and Virgo Collabora[ons, Phys. Rev. Lew. 116, no. 24, (2016) Ground exp.: LIGO[USA], KAGRA[JPN], VIRGO[ITA FRA], Just now observing GWs directly from astronomical phenomena such as the binary of neutron stars, black holes, etc. The era of GW astronomy will come true! Future space exp.: elisa[eu], DECIGO[JPN], Will be exploring phenomena at the very early stage of the Universe such as electroweak phase transi[on, cosmic infla[on, etc. We expect GWs as a new technique to explore the BSM, in addi[on to the collider experiment! 5 /18

9 Probing the first order electroweak phase transi5on by measuring gravita5onal waves in scalar extension models Contents Motivation: Physics behind the EWSB Electroweak Baryogenesis - 1 st order phase transition (1stOPT) hhh coupling & GWs GWs from 1stOPT Models of 1stOPT ( O(N) model & Higgs singlet model ) - Detectability at colliders and GW interferometers 1 /18

10 GWs from 1 st OPT Origin of GWs from 1stOPT Expanding bubbles of the broken phase C.Caprini et al., JCAP1604, 001 (2016) [review] r 0 : size of cri[cal bubble Bubble is spherical No GW occurs 6 /18

11 GWs from 1 st OPT Origin of GWs from 1stOPT C.Caprini et al., JCAP1604, 001 (2016) [review] r 0 : size of cri[cal bubble Typical radius of colliding bubbles: Transi[on [me: Spherical symmetry is violated by bubble collisions 6 /18

12 GWs from 1 st OPT Origin of GWs from 1stOPT Magnetohydrodynamic turbulence in the plasma C.Caprini et al., JCAP1604, 001 (2016) [review] Sound waves (Compressional plasma) Bubble collision (Envelope approximation) 6 /18

13 GWs from 1 st OPT GWs from 1 st OPT (*)C.Caprini et al., arxiv: [astro-ph.co] Predic[on t ``Relic abundance of peak @ 7 /18

14 GWs from 1 st OPT GWs from 1 st OPT Model parameters Input ``Spherical bubble configura[on t r 0 : Cri[cal size of vacuum babble Search the escape point. : ini[al condi[on Eq. of mo[on: each 3-dim. Euclidean action: 8 /18

15 GWs from 1 st OPT GWs from 1 st OPT Model parameters (*)C.Caprini et al., arxiv: [astro-ph.co] Input Predic[on t ``Characteris[c parameters of GWs Plot * (Observable) α is defined as. (ρ rad is energy density of rad.) - Latent heat: cf. U=-F+T(dF/dT) β is defined as. ( : Bubble nucleation rate, H t : Hubble t ) 9 /18

16 Probing the first order electroweak phase transi5on by measuring gravita5onal waves in scalar extension models Contents Motivation: Physics behind the EWSB Electroweak Baryogenesis - 1 st order phase transition (1stOPT) hhh coupling & GWs GWs from 1stOPT Models of 1stOPT ( O(N) model & Higgs singlet model ) - Detectability at colliders and GW interferometers 1 /18

17 models of 1stOPT Models of 1 st OPT Higgs poten5al by high temperature approxima5on E : thermal coupling (the non-decoupling effects due to the addi[onal boson loop) e : non-thermal coupling (the field mixing of the Higgs boson with addi[onal scalar fields) 10 /18

18 models of 1stOPT - thermal effect Models of 1 st OPT Higgs poten5al by high temperature approxima5on E : thermal coupling (the non-decoupling effects due to the addi[onal boson loop) e : non-thermal coupling (the field mixing of the Higgs boson with addi[onal scalar fields) J.Kehayias and S.Profumo, JCAP1003, 003 (2010) As the simplest model, we have inves[gated the O(N) model. 10 /18

19 models of 1stOPT - thermal effect - O(N) model Models of 1 st OPT Higgs poten5al by high temperature approxima5on E : thermal coupling (the non-decoupling effects due to the addi[onal boson loop) e : non-thermal coupling (the field mixing of the Higgs boson with addi[onal scalar fields) ``O(N) model N iso-singlet fields with O(N) sym. M.Kakizaki, S.Kanemura, T.Matsui, Phys. Rev. D 92, no. 11, (2015) - O(N) is not broken Common mass of S i : - Model parameters: (N, m S, μ S ) - 1stOPT: 11 /18

20 models of 1stOPT - thermal effect - O(N) model - detectability at colliders & GW obser. -1 φ c /T c Δλ hhh & Ω GW h H 4 T T t 1 Μ S 2 0 ms GeV φ c T c 1.0 Excluded by unitarity bound Λ hhh O N Λ hhh SM N M.Kakizaki, S.Kanemura, T.Matsui, Phys. Rev. D 92, no. 11, (2015) 12 /18

21 models of 1stOPT - thermal effect - O(N) model - detectability at colliders & GW obser. -1 φ c /T c Δλ hhh & Ω GW h 2 ms GeV H 4 T T t 1 φ c T c 1.0 Μ S 2 0 Excluded by unitarity bound Λ hhh O N Λ hhh SM Β N= 1 m S GeV Μ S 2 0 For small m S, φ c /T c >1 cannot be sa[sfied N For larger m S, Γ/H 4 T=Tt =1 cannot be realized. M.Kakizaki, S.Kanemura, T.Matsui, Phys. Rev. D 92, no. 11, (2015) Α 12 /18

22 models of 1stOPT - thermal effect - O(N) model - detectability at colliders & GW obser. -2 φ c /T c Δλ hhh & Ω GW h H 4 T T t 1 Μ S 2 0 ms GeV φ c T c 1.0 Excluded by unitarity bound Λ hhh O N Λ hhh SM DECIGO [Class. Quant. Grav. 28, (2011)], N elisa [arxiv: ] M.Kakizaki, S.Kanemura, T.Matsui, Phys. Rev. D 92, no. 11, (2015) 12 /18

23 models of 1stOPT - thermal effect - O(N) model - detectability at colliders & GW obser. -2 Predic[on * φ c /T c Δλ hhh & Ω GW h 2 t (*)C.Caprini et al., arxiv: [astro-ph.co] N=1, 4, 12, 24, 60 DECIGO [Class. Quant. Grav. 28, (2011)], elisa [arxiv: ] M.Kakizaki, S.Kanemura, T.Matsui, Phys. Rev. D 92, no. 11, (2015) 13 /18

24 models of 1stOPT Models of 1 st OPT Higgs poten5al by high temperature approxima5on E : thermal coupling (the non-decoupling effects due to the addi[onal boson loop) e : non-thermal coupling (the field mixing of the Higgs boson with addi[onal scalar fields) 10 /18

25 models of 1stOPT - mixing effect Models of 1 st OPT Higgs poten5al by high temperature approxima5on E : thermal coupling (the non-decoupling effects due to the addi[onal boson loop) e : non-thermal coupling (the field mixing of the Higgs boson with addi[onal scalar fields) J.Kehayias and S.Profumo, JCAP1003, 003 (2010) As the simplest model, we have inves[gated the Higgs singlet model (HSM). 10 /18

26 models of 1stOPT - mixing effect - HSM Models of 1 st OPT Higgs poten5al by high temperature approxima5on E : thermal coupling (the non-decoupling effects due to the addi[onal boson loop) e : non-thermal coupling (the field mixing of the Higgs boson with addi[onal scalar fields) ``Higgs singlet model (HSM) K.Hashino, M.Kakizaki, S.Kanemura, T.Matsui, P.Ko, arxiv: Tadpole condi[ons - Diagonalized mass matrix in and - 1stOPT is calculated by two-field T. 14 /18

27 models of 1stOPT - mixing effect - HSM - constraints Higgs couplings: recent LHC data: (1σ; combina[on of ATLAS and CMS) [ATLAS-CONF ] Expected accuracy: 2%@HL-LHC 14TeV 3000k -1 [ ], 0.37% (0.51%) for κ Z (κ W )@ILC 500GeV 500k -1 [ ] Devia[on of hhh coupling from SM: Expected accuracy: 54%@HL-LHC 14TeV 3000k -1 [CMS-PAS-FTR ], 27%@ILC 500GeV 4000k -1 [ ], 16% (10%)@ILC 1TeV 2000k -1 (5000k -1 ) [ ] Benchmark points Constraints K. Fuyuto and E. Senaha, PRD 90, (2014) 15 /18

28 models of 1stOPT - mixing effect - HSM - detectability at colliders & GW obser. -1 K.Hashino, M.Kakizaki, S.Kanemura, T.Matsui, P.Ko, arxiv: DECIGO [Class. Quant. Grav. 28, (2011)], elisa [arxiv: ] elisa or DECIGO is capable of detec[ng GWs in the most of the HSM parameter region with 1 st OPT. 16 /18

29 models of 1stOPT - mixing effect - HSM - detectability at colliders & GW obser. -2 K.Hashino, M.Kakizaki, S.Kanemura, T.Matsui, P.Ko, arxiv: DECIGO [Class. Quant. Grav. 28, (2011)], elisa [arxiv: ] The synergy between the precision measurements of the Higgs boson couplings and GWs at future experiments are shown. 17 /18

30 Conclusions Exploring the structure of the Higgs sector is important to understand physics behind EWSB. We have inves[gated various models of 1stOPT. The strongly 1stOPT of EWSB can be tested by the measurements of various Higgs boson the hhh and space-based interferometers. 18 /18

31 Back Up 31 /18

32 Triple Higgs boson coupling measurements HL-LHC (14TeV, 3000k -1 ) Δλ hhh /λ hhh ~50%(gg hh) Snowmass Higgs working group, arxiv: [hep-ex] ILC1000-up (500/1000GeV, k -1 ) Δλ hhh /λ hhh ~10%(ee ννhh) K.Fujii et al., arxiv: [hep-ex] 32 /18

33 EWPT: Mul[-field analysis of EWPT K. Funakubo, S. Tao and F. Toyoda, Prog. Theor. Phys. 114, 369 (2005) (NMSSM) K. Fuyuto and E. Senaha, Phys. Rev. D 90, no. 1, (2014) (HSM) Diverse pawerns of the c, B I A D EW C EW phase needs to be the global min.: SYM II Public tool CosmoTransi[on (Python code) is used. 33 /18

34 Theore[cal constraints Perturba[ve unitarity: Vacuum stability: Landau pole: Oblique parameters (S, T, U): S. Baek, P. Ko, W. I. Park and E. Senaha, JHEP 1211, 116 (2012) 34 /18

35 Singlet extension of the SM (non-thermal) Poten[al A.Ashoorioon, T.Konstandin, JCAP0809, 022 (2008) An example of the paths (assump[on) 35 /18

36 Singlet extension of the SM (non-thermal) A.Ashoorioon, T.Konstandin, JCAP0809, 022 (2008) Results(, ) 36 /18

37 Model parameters Input GWs from 1 st OPT ``Defini[on of phase transi[on temperature T t Phase transi[on completes when the probability for the nuclea[on of 1 bubble per 1 horizon volume and horizon [me is of order 1. - Bubble nucleation rate: - 3-dim. Euclidean action: H K.Kohri et al., arxiv: T GeV (H: Hubble parameter) 37 /18

38 GWs from 1 st OPT Model parameters Input ``Defini[on of phase transi[on temperature T t Oct , 2016, the KIAS Behavior Workshop of S 3 /T 38 /18

39 GWs from 1 st OPT Model parameters Input ``Defini[on of phase transi[on temperature T t S / T Model parameters are constrained T (GeV) R.Apreda et al., NPB631, 342 (2002) Oct , 2016, the KIAS Behavior Workshop of S 3 /T 39 /18

40 Behavior of β in relic abundance of GWs M.Kamionkowski, PRD49, 2837 (1994) Wave eq. from Einstein eq. in weak field approxima[on Stochas[c backgrounds of gravita[onal waves Because the characteris[c scale is, 40 /18

41 Origins of GWs from EWPT C.Caprini et al., arxiv: [astro-ph.co] (review) We improve our analysis in accordance with the recent simula[on result. 41 /18

42 Recent work of other souse of GW sound wave M.Hindmarsh, et al., PRL 112, (2014); arxiv: [astro-ph.co]. 42 /18

43 Origins of GWs from EWPT C.Caprini et al., arxiv: [astro-ph.co] (review) Vacuum bubble velocity v b Efficiency factor κ(v /18

44 Origins of GWs from EWPT C.Caprini et al., arxiv: [astro-ph.co] (review) Vacuum bubble velocity v b Efficiency factor κ(v b, α) J.R.Espinosa, et al, JCAP 1006, /18

45 Origins of GWs from EWPT C.Caprini et al., arxiv: [astro-ph.co] (review) Vacuum bubble velocity v b Efficiency factor κ(v b, α) J.R.Espinosa, et al, JCAP 1006, 028 (2010) The frac[on of bulk mo[on from the bubble walls The result from resent simula[on Hindmarsh, Huber, Rummukainen, Weir, PRD 92, no. 12, /18

46 (α, β[lde) (f, Ω GW h 2 ) new GWh Β 10 3, T t 50 GeV Α Frequency Hz T t 50 GeV Β 46 /18

47 (α, β[lde)_exp. by New spectra (T t =50GeV) sw HT t = 50 GeV) DECIGO Correlation 1 cluster env HT t = 50 GeV) MHD turb HT t = 50 GeV) DECIGO Correlation 10 4 b é b é b é elisa C1 C2 C3 C4 Pre a elisa C1 C2 C a elisa C1 DECIGO Correlation C a 47 /18

48 (α, β[lde)_exp. by New spectra (T t =100GeV) 10 6 sw HT t = 100 GeV) 10 6 env HT t = 100 GeV) 10 6 MHD turb HT t = 100 GeV) 10 5 DECIGO Correlation cluster 10 4 DECIGO Correlation 10 4 b é b é b é DECIGO Correlation 10 2 elisa C1 C2 C3 C4 Pre a 10 2 elisa C1 C2 C a 10 2 elisa C1 C2 C a 48 /18

49 Proper[es of the representa[ve elisa configura[ons C.Caprini et al., arxiv: [astro-ph.co] 49 /18

50 Efficiency factor κ(v b, α) J.R.Espinosa, et al, JCAP 1006, 028 (2010) 50 /18

51 J.R.Espinosa, et al J.R.Espinosa, et al., JCAP 1006, 028 (2010) ξ J is same as our v b (α) Κ Our calcula[on Ξ w J.M.No, PRD 84, (2011) 51 /18

52 Contour plot of α on (ξ w, v + ) plane α is given by effec[ve poten[al. Diffusion upper bound of EWBG EWBG requires small ξ w GW requires large J.M.No, PRD84, (2011) 52 /18

53 Contour plot of v + on (ξ w, α) plane α is given by effec[ve poten[al. EWBG requires small ξ w GW requires large J.M.No, PRD84, (2011) 53 /18

54 Foreground noise from white dwarf binaries R.Schneider, S.Marassi, V.Ferrari, Class. Quant. Grav. 27, (2010) 54 /18