ICAN: High Energy physics, Dark Matter and Dark Energy. Michel Spiro
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1 ICAN: High Energy physics, Dark Matter and Dark Energy Michel Spiro
2 _I Brout Englert, Higgs mechanism gives mass to particles
3 PLANCK image of the early universe (2.7 K map with 10-5 level inhomogeneities) La France et le CERN / décembre
4 BICEP2 Gravitational waves: confirms the standard lore of «big-bang» inflation at GeV
5 A new type of matter: «dark matter» A dominant enigmatic «substance»: «dark energy» Heavy Elements : 0.03% Neutrinos : 0.3% Stars 0.5% Gas H + HE 4% Dark Matter Dark Energy Michel Spiro, Santiago de Compostella, 20/11/09
6 The Acceleration of the Universe: dark energy (Supernovae, CMB, BAO ) Examples of type 1a supernovae Thermonuclear detonation of white dwarf High-redshift supernovae are systematically fainter than expected based on extrapolation of low-redshift sources. Must be further away than expected. So need an effect to overcome the tendency of gravity to slow down the expansion.
7 DARK MATTER Dark matter has already been discovered through Galaxy clusters Galactic rotation curves Weak lensing Strong lensing Hot gas in clusters Bullet Cluster Supernovae CMB, BAO Nucleosynthesis We are entering the decade of dark matter identification (it cannot be ordinary matter)
8 Origin of mass of elementary particles (neutrinos?) What is the nature of Dark Matter (supersymmetric particles, axions)? What is the nature of Dark Energy (Vacuum energy or space-time curvarure)? Where has all antimatter gone? (study of ultra cold antihydrogen atoms ) Enigmatic neutrinos 8 Random occurrences or new laws?
9 dark energy vs cosmological constant
10 Entering a new era for basic science LHCb CMS ATLAS The Higgs boson and the Lord of the Rings + Brout Englert LHC ALICE LHC ring : 27 km circumference
11 The study of elementary particles and fields and their interactions gauge x8 In 50 years, we ve come a long way, but there is still much to learn
12 La France et le CERN / décembre
13 13
14 VACUUM PHASE TRANSITION
15 Brout, Englert and Higgs mechanism What is vacuum? Full of virtual particles (quantum fluctuations): quasi medium Higgs virtual particles induce vacuum viscosity Vacuum Mexican hat potential shape! Plus existence of a Higgs-particle of mass < 1 TeV, accessible to LHC...
16 09/05/2014 IZEST-Jerusalem U Probing the quantum vacuum with high intensity lasers, a step towards understanding dark energy?
17 Questions on the HIGGS boson mass: On one hand the Higgs boson has a mass, not only in the allowed range by the Standard Model (below 1 TeV) but at the exact place where the Standard Model can be extrapolated up to GeV GUT or inflation scale where it develops some meta stability (inflaton)? On the other hand, quantum corrections to the Higgs mass in the Standard Model would naturally bring the Higgs mass to the inflation scale! Does supersymmetry <10 TeV (no sign yet!!) stabilize the Higgs mass at 126 GeV by cancellations of the corrections? The Higgs boson looks like an ice cube in the fire!
18 Summary of forces LHC 10 3 GeV GeV GeV
19 Dark matter. We know neither what the dark energy or the dark matter is A particle relic from the Big Bang is strongly implied for DM WIMPs (Lightest Supersymmetric Particle)? Axions? (an alternative to supersymmetry for dark matter)
20 1. Particle Dark Matter: supersymmetric neutralinos at GeV to 10 TeV scale Stable, TeV-scale particle, electrically neutral, only weakly interacting No such candidate in the Standard Model Lightest Supersymmetric Particle (LSP): superpartner of a gauge boson in most models LSP a perfect candidate for WIMP CDMS-II Detect Dark Matter to see it is there. Produce Dark Matter in accelerator experiments to see what it is.
21 Detection of supersymmetric Dark Matter: neutralinos Direct detection CDMS-II, Edelweiss, DAMA, GENIUS, etc Indirect detection SuperK, AMANDA, ICECUBE, Antares, etc complementary techniques are getting into the interesting region of parameter space
22 ? HL-LHC (3000 fb -1 ) LHC TeV (300 fb -1 ) LHC 7-8 TeV (30 fb -1 ) Samivel
23 Vision for next machine at CERN, after LHC to be decided around e+e- 500 GeV SC cavities Mature Japan? 2020? e+e- 3 TeV, Feasibility Study Klystrons, 2 beam acceleration, plasma? High Energy LHC 30 TeV New Idea (Nb3Sn) Or even 100 TeV 100 km new tunnel
24
25 Chirped Pulse Amplification D. Strickland and G. Mourou fs 4 09/05/2014 IZEST-Jerusalem U
26 Relativistic Rectification (Wake-Field Tajima, Dawson) F Bz æ = qç v è c Ù B ö ø Es + - v ÙB 1) pushes the electrons. 2) The charge separation generates an electrostatic longitudinal field. (Tajima and Dawson: Wake Fields or Snow Plough) E s = cgm ow p = 4pgm e o c 2 n e 3) The electrostatic field 09/05/2014 E s» E L IZEST-Jerusalem U
27 ICAN (European Project) CAN Coherent Amplification Network G. Mourou, W. Brocklesby, J. Limpert, T. Tajima, Nature Photonics April 2013 «The future of Acceletaor is Fiber» 09/05/2014 IZEST-Jerusalem U
28 LMJ/NIF, 2MJ, 3B Vacuum Polarization E p =m p c 2 MJ kj XCELS IZEST C 3 TeV GeV ELI, kj.3 B E e =m 0 c 2 J MeV mj ev ICUIL 2012 Mourou
29 G. Mourou
30 2. AXIONS: very light particles Strongly motivated by the strong CP problem 4m Motivates introduction of the axion (sub ev), which couples to two photons
31 Degenerate Four-Wave Mixing (DFWM) Laser-induced nonlinear optics in vacuum (cf. Nonlinear optics in crystal) 2w, xw Decay into (4-x)ω can be induced by frequency-mixing K.Homma, D.Habs, T.Tajima Appl. Phys. B (2012) xw, 2w +z w 0 (4-x)ω=2w+2w-xw resonance (signal) ~ N 1 N 2 N 3 / τ 2w, xw Sweep by arbitrary frequency xw. Wirth et al. (Science 2011: synthesized light transients) 31
![Strength of coupling [1/GeV] Photon mixer](/docs-images/85/92726117/images/32-0.jpg "to new fields: Dark Matter and Dark Energy")
32 Strength of coupling [1/GeV] Photon mixer to new fields: Dark Matter and Dark Energy in a single shot (with rep-rate such as ICAN/IZEST, far lower detection limit possible) SHG 200J 15fs DFWM 200J 1.5ns DFWM 200J 15fs. IZEST QCD axion (Dark matter) Gravitational Coupling(Dark Energy) K.Homma, D.Habs, T.Tajima (2012) mass of coupling [ev] 32
33 Dark matter and Dark Energy Two major evidences for physics beyond the standard model of particle physics and maybe beyond the standard model of cosmology Supersymmetry, axion searches and probing quantum vacuum are the main avenues to tackle these issues Affordable future accelerators together with ultra high intensity lasers will be crucially needed. The future of basic knowledge is at stake.
34
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