Higgs Fizz in the Big Bang

Transcription

1 Higgs Fizz in the Big Bang Mark Hindmarsh Department of Physics & Astronomy University of Sussex and Helsinki Institute of Physics & Dept of Physics, University of Helsinki Department of Physics Colloquium, University of Helsinki 18. toukokuuta 2018

2 In the beginning there was a duck. A scaup

3 The beginning according to Kalevala The duck laid 6 eggs on Ilmatar s knee. An egg broke. The halves of the eggshell became heaven and earth. The white became the moon and the yolk the sun.

4 The science of the beginning Begins with Einstein General Theory of Relativity (1915)

5 General Relativity A theory of gravity Space and time are linked and dynamical Spacetime tells matter how to move, matter tells spacetime how to curve John Wheeler Bending of starlight by sun observed 1919 PhysicsOfTheUniverse.com

6 The birth of modern cosmology Friedmann (1922) Lemaître (1927) From General Relativity: the theory of a universe containing uniformly distributed matter

7 Friedmann-Lemaître cosmology In a universe filled with matter, space expands Distant objects recede Recession velocity proportional to distance Wavelength of light stretched by expansion cosmological redshift PhysicsOfTheUniverse.com

8 The reception Your calculations are correct, but your physics is atrocious.

9 The beginning of the Big Bang Alpher and Gamow (1948) Going back in time: Density gets larger Temperature gets bigger Early Universe was HOT Evidence: cosmic microwaves (relic heat) proportion of 4 He, D, 3 He, 7 Li At s particle energy ~ 1 TeV protons in LHC have 13 TeV Light had travelled only 1 mm Expansion: 1 mm then becomes 1 billion km now George Gamow Ralph Alpher

10 How do particles get mass? All elementary particles (bar photon and gluon) have mass. Q: How do they get mass? A: From the Higgs field The Higgs particle `is a wave in the Higgs field The photon `is a wave in the electromagnetic field

11 The Higgs field and particle Higgs: scalar field manifests itself as a particle Predicted: 1964 Brout, Englert Higgs Guralnik, Hagen, Kibble Discovered: 2012 mass 125 GeV Finding the particle completed the Standard Model of Particle Physics (developed in 60s and 70s) Standard Model t-shirt (CERN)

12 The Standard Model and cosmology Energy density in particles mass energy m(φ) kinetic energy Energy density in Higgs field potential energy density V(φ) Hot/dense enough gas of particles reduces mass energy by forcing the Higgs field to zero Particles are massless at high temperature Mass turns on at around 10 ps Phase transition in the early universe (Kirzhnits 1972) Higgs field energy density (GeV 4 ) x Higgs field value (GeV) D A Kirzhnits

13 Phase transitions Water has phase transitions Boiling: liquid to vapour Condensing: vapour to liquid Higgs field turning on is a phase transition Temperature: K Water: at high pressure there is no distinction between liquid and gas: Supercritical fluid Which one is Higgs? Pressure liquid gas Temperature Supercritical fluid

14 Standard Model phases Low temperature: massive particles Higgs phase High temperature: massless particles force-carrying Z, W particles become like photon symmetric phase SM: no distinction SM is like a supercritical fluid Kajantie, Laine, Rummukainen, Shaposhnikov 1996 Higgs mass "supercritical" 125 GeV 75 GeV Higgs phase "condensation" Symmetric phase Temperature

15 Beyond the Standard Model Most particle physicists think there is more to discover, e.g: Dark matter Matter/antimatter Higgs mass puzzle Why 3 families A first order phase transition is a signal of new physics Supersymmetry Force-carrying particles (boson) paired with a matter particle (fermion) Dark matter particle and many more Composite Higgs Higgs is like a pion More forces more bosons More dimensions Elementary strings CMS detector, LHC

16 Little bangs in the Big Bang? A Higgs fizz would make loud sound in the hot plasma Colliding sound waves make gravitational waves Can they be detected? Can we extract information about the phase transition? Energy density as transition proceeds David Weir, U. Helsinki Hindmarsh, Huber, Rummukainen, Weir

17 Gravitational waves Predicted by Einstein, 1916 Generated by accelerating, asymmetric mass-energy Sources we know about: binary compact objects (neutron stars, black holes, white dwarves);supernovae and sources we don t: e.g. violent events in the very early Universe

18 Nerdy knowledge nugget You can see gravity waves in Brighton! Here they are! Water waves are gravity waves Gravity waves are not gravitational waves

19 Detecting gravitational waves Compare distances between test masses in two directions with laser interferometer Gravitational wave alternately stretches and squeezes the two arms y x LIGO Strain sensitivity: (100 Hz) Changes in arm length m LIGO

20 GW the firstwaves GW source GRAVITATIONAL mini-symposium on Thursday 31th May 2018 Rainer Weiss Nobel prize 2017 Massachusetts Institute of Technology on behalf of the LIGO Scientific Collaboration The beginnings of gravitational wave astronomy Mark Hindmarsh University of Sussex/University of Helsinki Observing the early Universe with gravitational waves Norbert Langer University of Bonn The astounding evolution of massive binary stars towards merging black holes Stephen Smartt Queen's University Belfast Kilonovae and the birth of multi-messenger astronomy Schedule 10:00 10:10 Welcome (Kaarle Hämeri) 10:10 11:00 Rainer Weiss 11:00 11:30 Norbert Langer 11:30 12:00 Coffee 12:00 12:30 Stephen Smartt 12:30 13:00 Mark Hindmarsh Merger of two black holes Register 6 confirmed detections including a binary neutron star LIGO CALTECH/MIT PLACE KUMPULA CAMPUS, EXACTUM A111 ADDRESS GUSTAF HÄLLSTRÖM ST. 2 CONTACT emilia.kilpua@helsinki.fi

21 Gravitational wave spectrum NASA

22 Gravitational waves from the early universe Events at time t generate waves with minimum frequency f 1/t (Hubble rate) Redshifted to a frequency now: f 0 = (a(t)/a(t 0 ))f Minimum frequencies (redshifted Hubble rates): Event Time/s Temp/GeV Temp/K f 0 /Hz QCD transition EW transition ? Start of Hot Big Bang (end of inflation)

23 Gravitational wave spectrum Higgs transition NASA

24 Laser Interferometer Space Antenna White dwarves Black holes Galaxy mergers Extreme gravity TeV-scale early Universe LISA LISA sensitivity Launch by year mission (up to 10 years) 2.5M km arms Science objectives:

25 First order phase transitions redux Steinhardt 84, Enqvist et al 92 Ignatius et al 94, Espinosa et al 2010 Four numbers describe transition: α = ( Latent heat )/(Total enthalpy) b = transition rate v w = Bubble wall speed H * = Hubble rate at nucleation Derived parameters: R * = mean bubble separation (~v w /b) K = fluid kinetic energy fraction (depends on a, v w ) Fractional energy density in GWs: GW (H a )(H b )K 2 Timescales t a and t b Duration of stresses Coherence time of stress fluctuations K vw c < s vw n =1.0 n =0.3 n =0.1 n =0.03 n = v w > c s vw > c s

26 Direct numerical simulation of an early Ingredients: Higgs field universe phase transition + r = W + V i ) η coupling to fluid (models energy transfer, friction) Relativistic fluid Ė i (EV i )+P [Ẇ i(wv i )] E energy density, Z i momentum density, V i velocity, W γ-factor Discretisation W ( + V i )= W 2 ( + V i ) 2. Ż i j (Z i V j )+@ i @ i = W ( + V j )@ i. ḧ ij r 2 h ij = 16 GT TT ij Ignatius et al (1994), Kurki-Suonio, Laine (1996) Wilson & Matthews (2003) Different approach: Giblin, Mertens (2013) Garcia-Bellido, Figueroa, Sastre (2008)

27 PRACE campaign Preparatory: 1M hrs CSC, Finland 2015/6: 17M CPU-hours Tier-0 (Hazel Hen, Stuttgart) lattice on 24k cores Aim: GW power spectrum d gw d ln f = 1 d gw tot d ln f = 8 2 3H 2 f 3 S h (f) Hindmarsh, Huber, Rummukainen, Weir 2017 Fluid kinetic energy in slice ( )

28 GW power spectra: detonation (H t) 1 (H R ) 1 d GW/d log k Transition strength: a = 0.01 Wall speed: v w = /T c 2000/T c 3000/T c 4000/T c 5000/T c k kr Peak at kr * ~ 10 Approx k -3 spectrum at high k Mean bubble separation: R * = 1900/T c Hindmarsh, Huber, Rummukainen, Weir (2017)

29 Gravitational waves from a vacuum phase transition Extreme supercooling: energy-momentum dominated by order parameter (Higgs field) Phase boundary keeps accelerating: v w 1 Cutting, Hindmarsh, Weir 2018 Higgs energy density (blue) Gravitational wave energy density (red)

30 LISA prospects for EW phase transition gw(f) c.f. Caprini et al (2015) [LISA Cosmology Working Group] f (Hz) LISA standard sensitivy LISA power law sensitivy Galactic binaries BH binaries MBH binaries GNMSSM (A) Higgs portal (A) 2HDM (C) SM + h 6 (A) SM + dilaton (B) Model T n /GeV a b/h n v w GNMSSM A Higgs portal A HDM C SM + h 6 A SM + dilaton B

31 Shocks and turbulence Future challenges Resolve disagreement between models Magnetic field dynamo Calculations of thermodynamic parameters from underlying models: α = ( Latent heat )/(Total enthalpy) b = transition rate v w = Bubble wall speed H * = Hubble rate at nucleation Correlations with collider (LHC ) data Distinguishing phase transitions from astrophysical GW foregrounds Aim: measure (α, b, v w, H * ) with GWs LISA Cosmology Working Group, Helsinki, June ma0 (GeV) m H0 (GeV) Shocked sound (Pen, Turok 2015) Andersen et al 2017

32 Summary Particle physics + cosmology: phase transitions in the early Universe Higgs field may have turned on with a fizz at s Sound of the fizz makes gravitational waves GWs have information about the phase transition We can look for the gravitational waves with LISA launch scheduled for 2034 look for merging black holes at galactic centres probe the Universe at 10 trillionths of a second old Search for gravitational waves from a Higgs phase transition complements hunt for new physics at LHC