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Mirror Matter As Dark Matter ...And Ordinary – Mirror

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Mirror Matter As Dark Matter ...And Ordinary – Mirror Mirror Matter as Dark Matter ... ... and ordinary { mirror particle mixings Mirror Matter as Dark Matter ... Zurab Berezhiani ... and ordinary { mirror particle mixings Summary Mirror Matter: general questions Chapter I: ordinary { mirror Zurab Berezhiani particle mixings Chapter II: neutron { mirror University of L'Aquila and LNGS neutron mixing Chapter III: n n and − 0 Particle Physics with Neutrons at the ESS, UHECR Nordita, 10-14 Dec. 2018 Contents Mirror Matter as Dark Matter ... ... and ordinary { mirror particle mixings Zurab Berezhiani Summary 1 Mirror Matter: general questions Mirror Matter: general questions Chapter I: ordinary { mirror 2 Chapter I: ordinary { mirror particle mixings particle mixings Chapter II: neutron { mirror neutron mixing 3 Chapter II: neutron { mirror neutron mixing Chapter III: n n0 and UHECR− 4 Chapter III: n n0 and UHECR − Chapter I Mirror Matter as Dark Matter ... ... and ordinary { mirror particle mixings Zurab Berezhiani Introduction Summary Mirror Matter: general questions Chapter I: ordinary { mirror particle mixings Mirror Matter: generalities Chapter II: neutron { mirror neutron mixing Chapter III: n n0 and UHECR− Bright & Dark Sides of our Universe Mirror Matter as Todays Universe: flat Ωtot 1 (inflation) ... and multi-component: Dark Matter ... ≈ ΩB 0:05 observable matter: electron, proton, neutron ! ... and ordinary { ' mirror particle ΩD 0:25 dark matter: WIMP? axion? sterile ν? ... mixings ' Zurab Berezhiani ΩΛ 0:70 dark energy: Λ-term? Quintessence? .... ' 3 Summary ΩR < 10− relativistic fraction: relic photons and neutrinos Mirror Matter: general questions Matter { dark energy coincidence: ΩM =ΩΛ 0:45, (ΩM = ΩD + ΩB ) 3 ' Chapter I: ρΛ Const., ρM a− ; why ρM /ρΛ 1 { just Today? ordinary { mirror ∼ ∼ ∼ particle mixings Antrophic explanation: if not Today, then Yesterday or Tomorrow. Chapter II: neutron { mirror neutron mixing Baryon and dark matter Fine Tuning: ΩB =ΩD 0:2 3 3 ' Chapter III: ρB a− , ρD a− : why ρB /ρD 1 - Yesterday Today & Tomorrow? n n0 and ∼ ∼ ∼ UHECR− Baryogenesis requires BSM Physics: (GUT-B, Lepto-B, AD-B, EW-B ...) Dark matter requires BSM Physics: (Wimp, Wimpzilla, sterile ν, axion, ...) Different physics for B-genesis and DM? Not very appealing: looks as Fine Tuning B-genesis and DM require new physics: but which ? Why ΩD =ΩB 1 ? ∼ Mirror Matter as Visible matter from Baryogenesis ( Sakharov) Dark Matter ... B (B L) & CP violation, Out-of-Equilibrium ... and ordinary { − 9 mirror particle ρB = mB nB , mB 1 GeV, η = nB =nγ 10− mixings ' ∼ Zurab Berezhiani η is model dependent on several factors: coupling constants and CP-phases, particle degrees of freedom, Summary Mirror Matter: mass scales and out-of-equilibrium conditions, etc. general questions Chapter I: Dark matter: ρD = mX nX , but mX = ? , nX = ? ordinary { mirror particle mixings and why mX nX = 5mB nB ? Chapter II: neutron { mirror nX is model dependent: DM particle mass and interaction strength neutron mixing (production and annihilation cross sections), freezing conditions, etc. Chapter III: n n0 and UHECR− 4 Axion ma meV na 10 n { CDM ∼ ∼ γ Neutrinos m eV n n { HDM ( ) ν ∼ ν ∼ γ Sterile ν 3 × 0 mν0 keV nν0 10− nν { WDM ∼ ∼ 3 WIMP mX TeV nX 10− nB { CDM ∼ ∼ 12 WimpZilla mX ZeV nX 10− nB { CDM ∼ ∼ How these Fine Tunings look ... Mirror Matter as Dark Matter ... B-genesis + WIMP B-genesis + axion B-cogenesis ... and ordinary { mirror particle 40 B"genesis Ε ... 40 B-genesis HΕ ...L 40 B-genesis HΕ ...L mixings CP CP CP ΡB ΡB ΡB Zurab Berezhiani 20 ! # 20 20 DM"freezing Σann... # L L 4 4 4 0 0 0 GeV GeV GeV " ! # ΡDM -4 ΡDM -4 Ρ "4 Ρ Ρ Summary Ρ 'a ΡDM Ρrad~a Ρrad~a ! rad H H Log -20 Log -20 Log -20 Mirror Matter: "3 % -3 M=R -3 M=R general questions Ρmat'a M R Ρmat~a Ρmat~a -40 Ρ& -40 ΡL -40 ΡL Chapter I: ordinary { mirror -60 Today -60 Today -60 Today particle mixings -25 -20 -15 -10 -5 0 -25 -20 -15 -10 -5 0 -25 -20 -15 -10 -5 0 Log a a0 LogHaa0 L LogHaa0 L Chapter II: ! " # neutron { mirror neutron mixing mX nX mB nB mana mB nB mB0 nB0 mB nB Chapter III: ∼ 3 ∼ 13 ∼ mX 10 mB ma 10− mB mB mB n n0 and 0 UHECR− ∼ 3 ∼ 13 ∼ nX 10− nB na 10 nB nB0 nB Fine∼ Tuning? Fine∼ Tuning? Natural∼ ? Two different New Physics for B-genesis and DM ? Or co-genesis by the same Physics explaining why ΩDM ΩB ? ∼ Dark sector ... similar to our luminous sector? \Imagination is more important than knowledge." Albert Mirror Matter as For observable particles .... very complex physics !! Dark Matter ... G = SU(3) SU(2) U(1) ( + SUSY ? GUT ? Seesaw ?) ... and ordinary { × × mirror particle photon, electron, nucleons (quarks), neutrinos, gluons, W ± Z, Higgs ... mixings − long range EM forces, confinement scale ΛQCD, weak scale MW Zurab Berezhiani ... matter vs. antimatter (B-L violation, CP ... ) Summary ... existence of nuclei, atoms, molecules .... life.... Homo Sapiens ! Mirror Matter: general questions If dark matter comes from extra gauge sector ... it is as complex: Chapter I: G 0 = SU(3)0 SU(2)0 U(1)0 ? ( + SUSY ? GUT 0? Seesaw ?) ordinary { mirror × × photon0, electron0, nucleons0 (quarks0), W 0 Z 0, gluons0 ? particle mixings − Chapter II: ... long range EM forces, confinement at ΛQCD0 , weak scale MW0 ? neutron { mirror neutron mixing ... asymmetric dark matter (B0-L0 violation, CP ... ) ? Chapter III: ... existence of dark nuclei, atoms, molecules ... life ... Homo Aliens ? n n0 and UHECR− Let us call it Yin-Yang Theory in chinise, Yin-Yang means dark-bright duality describes a philosophy how opposite forces are ac- tually complementary, interconnected and interde- pendent in the natural world, and how they give rise E8 E80 to each other as they interrelate to one another. × SU(3) SU(2) U(1) + SU(3)0 SU(2)0 U(1)0 × × × × Mirror Matter as G G Dark Matter ... 0 Regular world × Mirror world ... and ordinary { mirror particle mixings Zurab Berezhiani Summary Mirror Matter: general questions Chapter I: ordinary { mirror particle mixings Chapter II: neutron { mirror Two identical gauge factors, e.g. SU(5) SU(5)0, with identical field neutron mixing • × contents and Lagrangians: tot = + 0 + mix Chapter III: L L L L n n0 and − Exact parity G G 0: no new parameters in dark Lagrangian 0 UHECR • ! L MM is dark (for us) and has the same gravity • MM is identical to standard matter, (asymmetric/dissipative/atomic) • but realized in somewhat different cosmological conditions: T 0=T 1. New interactions between O & M particles mix • L { All you need is ... M world colder than ours ! Mirror Matter as Dark Matter ... For a long time M matter was not considered as a real candidate for DM: ... and ordinary { naively assuming that exactly identical microphysics of O & M worlds mirror particle mixings implies also their cosmologies are exactly identical : Zurab Berezhiani eff eff T 0 = T , g 0 = g ∆Nν = 6:15 vs. ∆Nν < 0:5 (BBN) • ∗ ∗ ! Summary nB0 =nγ0 = nB =nγ (η0 = η) ΩB0 = ΩB vs. ΩB0 =ΩB 5 (DM) Mirror Matter: • ! ' general questions Chapter I: ordinary { mirror particle mixings But M World is OK if : Z.B., Comelli, Villante, 2001 Chapter II: neutron { mirror (A) after inflation M world was born colder than O world neutron mixing Chapter III: (B) all particle interactions between M and O sectors are so feeble that n n0 and UHECR− cannot bring them into equilibrium in later epochs (C) two systems evolve adiabatically when the universe expands (no entropy production) and their temperature ratio T 0=T remains nearly constant. If x = T 0=T 1, BBN is OK M world in Winter Z.B., Comelli, Villante, 2000 Mirror Matter as Dark Matter ... T 0 T 0 5 is enough to concord with the BBN limits and do not affect ... and ordinary { = < : 4 mirror particle standard primordial mass fractions: 75% H + 25% He. mixings (Cosmological limits are more severe, requiring T 0=T < 0:2 os so.) Zurab Berezhiani 4 In turn, for M world this implies helium domination: 25% H0 + 75% He0. Summary Mirror Matter: Because of T 0 < T , in mirror photons decouple much earlier than ordinary general questions photons, and after that M matter behaves for the structure formation and Chapter I: CMB anisotropies essentially as CDM. This concords M matter with ordinary { mirror particle mixings WMAP/Planck, BAO, Ly-α etc. if T 0=T < 0:25 or so. Chapter II: neutron { mirror Halo problem { if ΩB0 ΩB , M matter makes 20 % of DM, forming dark neutron mixing disk, while 80 % may' come from other type∼ of CDM (WIMP?) Chapter III: ∼ n n and But perhaps 100 % ? if Ω0 5Ω : { M world is helium dominated, and − 0 B B UHECR the star formation and evolution' can be much faster. Halos could be viewed as mirror elliptical galaxies, with our matter inside forming disks. Because of T 0 < T , the situationΩ B0 > ΩB becomes plausible in baryogenesis. So, M matter can be dark matter (as we show below) CMB and LSS power spectra 80 Mirror Matter as #M=0.25, $b=0.023, h=0.73, n=0.97 Dark Matter ... x=0.5, no CDM x=0.3, no CDM ) " x=0.2, no CDM ... and ordinary { 60 (µ Z.B., Ciarcelluti, Comelli, Villante, 2003 1/2 mirror particle ] ! 2 mixings / l C ) 40 1 + Zurab Berezhiani l ( l [ Summary 20 WMAP ACBAR Mirror Matter: 0 200 400 600 800 1000 1200 1400 general questions l 104 5 Chapter I: 10 ordinary { mirror 102 2df bin. particle mixings ) 3 c 4 p 0 M ) 10 ( 3 10 Chapter II: c 3 p h ) neutron { mirror M ( k ( -2 neutron mixing 3 P 10 h ) k "M=0.30,#b=0.001,h=0.70,n=1.00 ( 3 P 10 "M=0.30,#b=0.02,h=0.70,n=1.00 Chapter III: -4 10 "M=0.30,#b=0.02,h=0.70,x=0.2,no CDM,n=1.00 n n0 and "M=0.30,#b=0.02,h=0.70,x=0.1,no CDM,n=1.00 UHECR− "M=0.30,#b=0.02,h=0.70,x=0.2,#b’=#CDM,n=1.00 10-6 102 0.01 0.1 1.0 10 k/h (Mpc!1 0.01 0.10 ) k/h (Mpc%1) Acoustic oscillations and Silk damping at short scales: x = T 0=T < 0:2 Can Mirror stars be progenitors of gravitational Wave bursts GW150914 etc.
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