Getting antimatter out of dark matter: introduction to mirror (anti)world Getting antimatter out of dark matter: Zurab Berezhiani Summary introduction to mirror (anti)world Introduction Dark Matter Enigma Zurab Berezhiani Mirror Matter B-L violating processes and University of L'Aquila and LNGS origin of observable and dark matter Zurich, 27 Sept. 2016 Neutron{mirror neutron oscillation The neutron lifetime enigma Conclusions Contents Getting antimatter out of dark matter: introduction to mirror (anti)world 1 Introduction Zurab Berezhiani 2 Summary Dark Matter Enigma Introduction Dark Matter 3 Mirror Matter Enigma Mirror Matter 4 B-L violating B-L violating processes and origin of observable and dark matter processes and origin of observable and dark matter 5 Neutron{mirror neutron oscillation Neutron{mirror neutron oscillation 6 The neutron lifetime enigma The neutron lifetime enigma 7 Conclusions Conclusions Some epochal discoveries after 30's of XIX ... Getting antimatter out of Anti-matter, 1931-32 dark matter: introduction to mirror (anti)world Zurab Berezhiani Summary Dark matter , 1932-33 Introduction Dark Matter Enigma Mirror Matter Neutron, 1932-33 B-L violating processes and origin of observable and dark matter Neutron{mirror neutron oscillation Parity Violation, 1956-57 The neutron lifetime enigma Conclusions CP Violation, 1964 ...and a prophetic idea on the origin of matter Getting antimatter out of dark matter: introduction to mirror A dreamer ... Andrey Sakharov, 1967 (anti)world Zurab Berezhiani Matter (Baryon asymmetry) in the early universe Summary can be originated (from zero) by processes that Introduction Violate B (better B L) Dark Matter − Enigma Violate CP Mirror Matter and go out-of-equilibrium at some early epoch B-L violating processes and origin of observable and dark matter Neutron{mirror neutron oscillation I want to pose a question in this way: The neutron lifetime enigma Can the issues of the antimatter, dark matter, neutron, parity, Conclusions CP-violation, baryon violation and some other issues of Standard Model more intimately related ? Standard Model on T-shirts Getting antimatter out of dark matter: introduction to mirror (anti)world Zurab Berezhiani Summary Introduction Dark Matter Enigma Mirror Matter B-L violating processes and origin of observable and dark matter Neutron{mirror neutron oscillation The neutron lifetime enigma Fermions (= matter): quarks and leptons, 3 generations Conclusions Bosons (= interactions): gauge fields + God's particle { Higgs Standard Model vs. P, C, T and B & L Getting Fermions: antimatter out of dark matter: uL νL introduction to qL = ; lL = ; uR ; dR ; eR mirror dL eL (anti)world B=1/3 L=1 B=1/3 L=1 Zurab Berezhiani Summary Anti-Fermions: Introduction u¯ ν¯ q¯ = R ; l¯ = R ;u ¯ ; d¯ ; e¯ Dark Matter R d¯ R e¯ L L L Enigma R R Mirror Matter B=-1/3 L=-1 B=-1/3 L=-1 B-L violating processes and origin of SM = Gauge + Higgs + Yuk CPT is OK (Local Lagrangian) observable and L L L L dark matter ¯ Neutron{mirror P (ΨL ! ΨR )& C (ΨL ! ΨL) broken by gauge interactions neutron ; ; oscillation ¯ u d e CP (ΨL ! ΨR ) broken by complex Yukawas Y = Yij The neutron lifetime enigma ¯ ¯ ¯ ¯ ¯ (¯uLYuqLφ+dLYd qLφ+e ¯LYe lLφ)+(uR Yu∗q¯R φ+dR Yd∗q¯R φ+eR Ye∗lR φ) Conclusions There are no renormalizable interactions which can break B and L ! Good for our stability, Bad for baryogenesis Baryogenesis requires new physics: B & L can be violated only in higher order (non-renormalizable) terms Getting antimatter out of dark matter: 1 ¯ ¯ 2 M (lφ)(lφ) (∆L = 2) { neutrino (seesaw) masses mν v =M introduction to • ∼ mirror (anti)world Zurab Berezhiani L=2 Summary MM Introduction GL=2 NN Dark Matter l Enigma l l l Mirror Matter 1 B-L violating M5 (udd)(udd) (∆B = 2) { neutron-antineutron oscillation n n¯ processes and • ! origin of observable and dark matter u u Neutron{mirror B=2 neutron u u d d oscillation S MM S d GB=2 d The neutron NN lifetime enigma d d Conclusions d d can originate from new physics related to scale M vEW via seesaw Dark matter requires new physics Standard Model has no candidate for dark matter Getting massive neutrino (∼ 20 eV) was a natural \standard" candidate of "hot" antimatter out of dark matter (HDM) forming cosmological structures (Pencakes) { dark matter: introduction to but it was excluded by astrophysical observations in 80's, mirror (anti)world and later on by the neutrino experiments! { RIP Zurab Berezhiani In about the same period the BBN limits excluded dark matter Summary in the form of invisible baryons (dim stars, etc.) { RIP Introduction Dark Matter Then a new Strada Maestra was opened { USY Enigma { well-motivated theoretical concept promisingS to be a highway Mirror Matter for solving many fundamental problems, brought a natural and B-L violating processes and almost \Standard" candidate WIMP { undead, but looks useless origin of observable and dark matter Another well-motivated candidate, Axion, emerged from Peccei-Quinn Neutron{mirror neutron symmetry for solving strong CP problem { alive, but seems confused oscillation The neutron lifetime enigma All other candidates in the literature are ad hoc ! Conclusions Apart one exception { which may answer to tantalizing question: do baryogenesis and dark matter require two different new physics, or just one can be enough? Cosmic Concordance and Dark Side of the Universe Getting Todays Universe: flat Ωtot 1 (inflation) and multi-component: antimatter out of ≈ dark matter: Ω 0:05 observable matter: electron, proton, neutron B ' introduction to WIMP? axion? sterile ν? ... mirror ΩD 0:25 dark matter: (anti)world ' ΩΛ 0:70 dark energy: Λ-term? Quintessence? .... Zurab Berezhiani ' Matter { dark energy coincidence: ΩM =ΩΛ 0:45, (ΩM = ΩD + ΩB ) Summary 3 ' ρΛ Const., ρM a− ; why ρM /ρΛ 1 { just Today? Introduction ∼ ∼ ∼ Dark Matter Antrophic explanation: if not Today, then Yesterday or Tomorrow. Enigma Mirror Matter Baryon and dark matter Fine Tuning: ΩB =ΩD 0:2 3 3 ' B-L violating ρB a− , ρD a− : why ρB /ρD 1 - Yesterday Today & Tomorrow? processes and ∼ ∼ ∼ origin of observable and { How Baryogenesis could know about Dark dark matter Matter? popular models for primordial Ba- Neutron{mirror neutron ryogenesis (GUT-B, Lepto-B, Affleck-Dine oscillation B, EW B ...) have no relation to popular The neutron lifetime enigma DM candidates (Wimp, Wimpzilla, sterile ν, Conclusions axion, gravitino ...) { Anthropic? Another Fine Tuning in Particle Physics and Cosmology? Coincidence of luminous and dark matter fractions: why ΩD =ΩB ∼ 1 ? or why mB ρB ∼ mX ρX ? Getting Visible matter from antimatter out of Baryogenesis ( Sakharov) dark matter: B (B L) & CP violation, Out-of-Equilibrium introduction to − 9 mirror ρB = mB nB , mB 1 GeV, η = nB =nγ 10− (anti)world ' ∼ Zurab Berezhiani η is model dependent on several factors: coupling constants and CP-phases, particle degrees of freedom, Summary mass scales and out-of-equilibrium conditions, etc. Introduction Dark Matter Enigma Dark matter: ρD = mX nX , but mX = ? , nX = ? Mirror Matter nX is model dependent: DM particle mass and interaction strength B-L violating (production and annihilation cross sections), freezing conditions, etc. processes and origin of observable and 5 4 Axion m 10− eV n 10 n - CDM dark matter a ∼ a ∼ γ 1 Neutron{mirror Neutrinos mν 10− eV nν nγ - HDM ( ) neutron ∼ ∼ oscillation Sterile ν 3 × 0 mν0 10 keV nν0 10− nν - WDM The neutron ∼ ∼ lifetime enigma Para-baryons mB0 1 GeV nB0 nB - SIDDM Conclusions ' ∼ 3 WIMP m 1 TeV n 10− n - CDM X ∼ X ∼ B 14 14 WimpZilla m 10 GeV n 10− n - CDM X ∼ X ∼ B How these Fine Tunings look ... Getting antimatter out of dark matter: introduction to mirror (anti)world B-genesis + WIMP B-genesis + axion B-cogenesis Zurab Berezhiani 40 B"genesis ΕCP... 40 B-genesis HΕCP...L 40 B-genesis HΕCP...L ΡB ΡB ΡB Summary 20 ! # 20 20 DM"freezing Σann... # L L 4 4 4 Introduction 0 0 0 GeV GeV GeV " ! # ΡDM -4 ΡDM -4 Ρ "4 Ρ Ρ Ρ 'a ΡDM Ρrad~a Ρrad~a ! Dark Matter rad H H Log Log -20 Log -20 Enigma -20 "3 % -3 M=R -3 M=R Ρmat'a M R Ρmat~a Ρmat~a Mirror Matter -40 Ρ& -40 ΡL -40 ΡL B-L violating -60 Today -60 Today -60 Today processes and -25 -20 -15 -10 -5 0 -25 -20 -15 -10 -5 0 -25 -20 -15 -10 -5 0 Log a a LogHaa L LogHaa L origin of 0 0 0 observable and ! " # dark matter Neutron{mirror mX nX mB nB mana mB nB mB0 nB0 mB nB neutron ∼ 3 ∼ 13 ∼ oscillation mX 10 mB ma 10− mB mB0 mB ∼ 3 ∼ 13 ∼ The neutron nX 10− nB na 10 nB nB0 nB lifetime enigma Fine∼ Tuning? Fine∼ Tuning? Natural∼ ? Conclusions SU(3) SU(2) U(1) & SU(3)0 SU(2)0 U(1)0 × × × × Getting G G 0 antimatter out of Regular world × Mirror world dark matter: introduction to mirror (anti)world Zurab Berezhiani Summary Introduction Dark Matter Enigma Mirror Matter • Two identical gauge factors, e.g. SU(5) × SU(5)0, with identical field B-L violating contents and Lagrangians: L = L + L0 + L processes and tot mix origin of 0 0 observable and • Exact parity G ! G : no new parameters in dark Lagrangian L dark matter Neutron{mirror • M sector is dark (for us) and the gravity is a common force (with us) neutron oscillation • M matter looks as non-standard for dark matter but it is truly standard The neutron in direct sense, just as our matter (self-interacting/dissipative/asymmetric) lifetime enigma Conclusions • New interactions are possible between O & M particles Lmix • Natural in string/brane theory: O & M matters localized on two parallel 0 branes and gravity propagating in bulk: e.g.