Mirror World: visible/dark matter genesis

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1 Mirror World: visible/dark matter genesis neutrinos, neutrons etc. Zurab Berezhiani Università di L Aquila and LNGS, Italy DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 1/??

2 Standard Cosmological Paradigm Precision data on BBN, CMB, LSS, etc. lead to Standard Paradigm: The early Universe: multi-stage: Inflation (re)heating Friedmann epoch... Universe is flat and homogeneous... Adiabatic perturbations with nearly flat spectrum... Todays Universe: multi-component: visible matter, dark matter, dark energy... Ω tot 1 Universe is flat: ρ tot = ρ cr... Ω B 0.04 visible (Baryon) matter is a small fraction... Ω D 0.20 dark matter: WIMPS? Axions?... Ω Λ 0.75 dark energy: Λ-term? 5th-essence?... DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 2/??

3 Standard Cosmological Paradigm Precision data on BBN, CMB, LSS, etc. lead to Standard Paradigm: The early Universe: multi-stage: Inflation (re)heating Friedmann epoch... Universe is flat and homogeneous... Adiabatic perturbations with nearly flat spectrum... Todays Universe: multi-component: visible matter, dark matter, dark energy... Ω tot 1 Universe is flat: ρ tot = ρ cr... Ω B 0.04 visible (Baryon) matter is a small fraction... Ω D 0.20 dark matter: WIMPS? Axions?... Ω Λ 0.75 dark energy: Λ-term? 5th-essence?... Some unified picture? Well, not yet... the origin and nature of DM and DE remain open! DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 2/??

4 Coincidence & Fine Tuning Problems Cosmic coincidence of matter (Ω M =Ω D +Ω B ) and dark energy (Ω Λ ) : Ω M /Ω Λ 0.3 : ρ Λ Const., ρ M a 3. Why ρ M /ρ Λ 1 just Today? DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 3/??

5 Coincidence & Fine Tuning Problems Cosmic coincidence of matter (Ω M =Ω D +Ω B ) and dark energy (Ω Λ ) : Ω M /Ω Λ 0.3 : ρ Λ Const., ρ M a 3. Why ρ M /ρ Λ 1 just Today? Well, if not Today, then it would be Yesterday or Tomorrow... Anthropic "Our Universe is just lucky that someone can ask this..." or Voltairian "Everything goes in best ways in our best world..." DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 3/??

6 Coincidence & Fine Tuning Problems Cosmic coincidence of matter (Ω M =Ω D +Ω B ) and dark energy (Ω Λ ) : Ω M /Ω Λ 0.3 : ρ Λ Const., ρ M a 3. Why ρ M /ρ Λ 1 just Today? Well, if not Today, then it would be Yesterday or Tomorrow... Anthropic "Our Universe is just lucky that someone can ask this..." or Voltairian "Everything goes in best ways in our best world..." Miracle Fine Tuning between visible (Ω B ) and dark (Ω D ) matter : Ω B /Ω D 0.2 : ρ B a 3, ρ D a 3. Why then ρ B /ρ D 1 Yesterday, Today and Tomorrow? Visible matter ρ B from primordial Baryogenesis (GUT, Lepto-B, Affleck-Dine, EW,...) Dark matter ρ D emerges from quite a different mechanism (Axion, Wimpino, Penta-Wimp, Wimpzilla, gravitino...) DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 3/??

7 Coincidence & Fine Tuning Problems Cosmic coincidence of matter (Ω M =Ω D +Ω B ) and dark energy (Ω Λ ) : Ω M /Ω Λ 0.3 : ρ Λ Const., ρ M a 3. Why ρ M /ρ Λ 1 just Today? Well, if not Today, then it would be Yesterday or Tomorrow... Anthropic "Our Universe is just lucky that someone can ask this..." or Voltairian "Everything goes in best ways in our best world..." Miracle Fine Tuning between visible (Ω B ) and dark (Ω D ) matter : Ω B /Ω D 0.2 : ρ B a 3, ρ D a 3. Why then ρ B /ρ D 1 Yesterday, Today and Tomorrow? Visible matter ρ B from primordial Baryogenesis (GUT, Lepto-B, Affleck-Dine, EW,...) Dark matter ρ D emerges from quite a different mechanism (Axion, Wimpino, Penta-Wimp, Wimpzilla, gravitino...) Finest conspiracy across the Particle Physics and Cosmology? How Baryon Asymmetry knew about Dark Matter Nature? DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 3/??

8 Visible & dark matter Visible matter: ρ B = n B M N 10 7 GeV cm 3, M N 1 GeV nucleon mass, n B = Y B s 10 7 cm 3 : (today s 3n γ 10 3 cm 3 ) BBN, LSS & CMB: the baryon number/entropy density ratio Y B = n B /s ( Const. during Universe expansion) (GUT, Lepto)-Baryogenesis: Y B (ǫ CP /g ) D(k), ǫ CP CP violation parameter, g effective number of particle degrees of freedom at T = T B, k = Γ/H out-of-equilibrium parameter at T = T B DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 4/??

9 Visible & dark matter Visible matter: ρ B = n B M N 10 7 GeV cm 3, M N 1 GeV nucleon mass, n B = Y B s 10 7 cm 3 : (today s 3n γ 10 3 cm 3 ) BBN, LSS & CMB: the baryon number/entropy density ratio Y B = n B /s ( Const. during Universe expansion) (GUT, Lepto)-Baryogenesis: Y B (ǫ CP /g ) D(k), ǫ CP CP violation parameter, g effective number of particle degrees of freedom at T = T B, k = Γ/H out-of-equilibrium parameter at T = T B Dark matter: ρ D = n X M X GeV cm 3, LSS & CMB but M X =?, n X =? Axion : M X 10 5 ev; LSP/Bino.. : M X 1 TeV, Wimpzilla : M X GeV DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 4/??

10 B vs D Cosmological evolution of Baryon and dark matter densities: 40 B genesis Ε CP B genesis Ε CP Ρ B DM freezing Σ ann Ρ B Log Ρ GeV Ρ DM Ρ rad a 4 Log Ρ GeV Ρ DM Ρrad a 4-40 Ρ Ρ mat a 3 M R -40 Ρ Ρ mat a 3 M R -60 Today Log a a 0-60 Today Log a a 0 DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 5/??

11 Unified origin of VM and DM? 40 B genesis Ε CP Ρ B Log Ρ GeV Ρ DM Ρ rad a 4-40 Ρ Ρ mat a 3 M R -60 Today Log a a 0 ρ X /ρ B = M X n X /M N n B 1? DM properties are similar to VM properties: M X M N both fractions are generated by same mechanism: n X n B DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 6/??

12 Through the Looking-Glass Lewis Carroll Now, if you ll only attend, Kitty, and not talk so much, I ll tell you all my ideas about Looking-glass House. There s the room you can see through the glass that s just the same as our drawing-room, only the things go the other way... the books are something like our books, only the words go the wrong way: I know that, because I ve held up one of our books to the glass, and then they hold up one in the other room. I can see all of it all but the bit just behind the fireplace. I do so wish I could see that bit! I want so to know whether they ve a fire in the winter: you never can tell, you know, unless our fire smokes, and then smoke comes up in that room too but that may be only pretence, just to make it look as if they had a fire... How would you like to leave in the Looking-glass House, Kitty? I wander if they d give you milk in there? But perhaps Looking-glass milk isn t good to drink? Now we come to the passage: it s very like our passage as far as you can see, only you know it may be quite on beyond. Oh, Kitty, how how nice it would be if we could get through into Looking-glass House! Let s pretend there s a way of getting through into it, somehow, Kitty... Why, it s turning into a sort of mist now, I declare! It ll be easy enough to get through... Alice said this, and in another moment she was through the glass... she was quite pleased to find that there was a real fire in the fireplace... So I shall be as worm here as I was in my room, thought Alice: warmer, in fact, there ll be no one here to scold me away from the fire. DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 7/??

13 Mirror World Imagine a parallel hidden "Mirror" sector of particles, an exact duplicate of the observable sector. [Lee & Yang 56] [Kobzarev, Okun, Pomeranchuk 66] [Blinnikov, Khlopov 83] DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 8/??

14 Mirror World Imagine a parallel hidden "Mirror" sector of particles, an exact duplicate of the observable sector. [Lee & Yang 56] [Kobzarev, Okun, Pomeranchuk 66] [Blinnikov, Khlopov 83] Two identical gauge factors, G G, with the identical field contents and Lagrangians: L tot = L + L + L mix (exact parity under G G ) SM SM : SU(3) SU(2) U(1) SU(3) SU(2) U(1), or GUT GUT : SU(5) SU(5), SO(10) SO(10), etc. Can naturally emerge in string theory context: O & M matter fields are localized on two parallel branes (or on brane & antibrane) while gravity propagates in bulk (E 8 E 8 etc.) Mirror matter is dark for us, but we know all particle physics properties there no unknown parameters! DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 8/??

15 Mirror World Imagine a parallel hidden "Mirror" sector of particles, an exact duplicate of the observable sector. [Lee & Yang 56] [Kobzarev, Okun, Pomeranchuk 66] [Blinnikov, Khlopov 83] Two identical gauge factors, G G, with the identical field contents and Lagrangians: L tot = L + L + L mix (exact parity under G G ) SM SM : SU(3) SU(2) U(1) SU(3) SU(2) U(1), or GUT GUT : SU(5) SU(5), SO(10) SO(10), etc. Can naturally emerge in string theory context: O & M matter fields are localized on two parallel branes (or on brane & antibrane) while gravity propagates in bulk (E 8 E 8 etc.) Mirror matter is dark for us, but we know all particle physics properties there no unknown parameters! Spontaneously broken G G : M W M W [Z.B. & Mohapatra 95] shadow dark matter with rescaled spectrum [Z.B., Dolgov & Mohapatra 96] DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 8/??

16 Mirror Particles and Mirror Parity SU(3) SU(2) U(1) SU(3) SU(2) U(1) gauge (g, W, Z, γ) gauge (g, W, Z, γ ) & Higgs (φ) fields & Higgs (φ ) fields quarks (B=1/3) leptons (L=1) quarks (B =1/3) leptons (L =1) q L = (u, d) t L l L = (ν, e) t L q L = (u, d ) t L l L = (ν, e ) t L u R d R e R u R d R e R quarks (B=-1/3) leptons (L=-1) quarks (B =-1/3) leptons (L =-1) q R = (ũ, d) t R lr = ( ν, ẽ) t R q R = (ũ, d ) t R l R = ( ν, ẽ ) t R ũ L dl ẽ L ũ L d L ẽ L L Yuk = f L Y f L φ + f R Y f R φ L Yuk = f L Y f L φ + f R Y f R φ DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 9/??

17 Mirror Particles and Mirror Parity SU(3) SU(2) U(1) SU(3) SU(2) U(1) gauge (g, W, Z, γ) gauge (g, W, Z, γ ) & Higgs (φ) fields & Higgs (φ ) fields quarks (B=1/3) leptons (L=1) quarks (B =1/3) leptons (L =1) q L = (u, d) t L l L = (ν, e) t L q L = (u, d ) t L l L = (ν, e ) t L u R d R e R u R d R e R quarks (B=-1/3) leptons (L=-1) quarks (B =-1/3) leptons (L =-1) q R = (ũ, d) t R lr = ( ν, ẽ) t R q R = (ũ, d ) t R l R = ( ν, ẽ ) t R ũ L dl ẽ L ũ L d L ẽ L L Yuk = f L Y f L φ + f R Y f R φ L Yuk = f L Y f L φ + f R Y f R φ D-parity: L L, R R, φ φ Y = Y DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 9/??

18 Mirror Particles and Mirror Parity SU(3) SU(2) U(1) SU(3) SU(2) U(1) gauge (g, W, Z, γ) gauge (g, W, Z, γ ) & Higgs (φ) fields & Higgs (φ ) fields quarks (B=1/3) leptons (L=1) quarks (B =1/3) leptons (L =1) q L = (u, d) t L l L = (ν, e) t L q L = (u, d ) t L l L = (ν, e ) t L u R d R e R u R d R e R quarks (B=-1/3) leptons (L=-1) quarks (B =-1/3) leptons (L =-1) q R = (ũ, d) t R lr = ( ν, ẽ) t R q R = (ũ, d ) t R l R = ( ν, ẽ ) t R ũ L dl ẽ L ũ L d L ẽ L L Yuk = f L Y f L φ + f R Y f R φ L Yuk = f L Y f L φ + f R Y f R φ D-parity: L L, R R, φ φ Y = Y M-parity: L R, R L, φ φ Y = Y DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 9/??

19 O & M interactions besides gravity Higgs-Higgs quartic: λ(φ φ)(φ φ ); BBN: λ < safe in SUSY : W = 1 M (φ uφ d )(φ uφ d ) DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 10/??

20 O & M interactions besides gravity Higgs-Higgs quartic: λ(φ φ)(φ φ ); BBN: λ < safe in SUSY : W = 1 M (φ uφ d )(φ uφ d ) Photon-photon kinetic mixing: εf µν F µν ; BBN: ε < safe in GUT : L α GΣΣ 4πM 2 G µν G µν [Glashow 86] DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 10/??

21 O & M interactions besides gravity Higgs-Higgs quartic: λ(φ φ)(φ φ ); BBN: λ < safe in SUSY : W = 1 M (φ uφ d )(φ uφ d ) Photon-photon kinetic mixing: εf µν F µν ; BBN: ε < safe in GUT : L α GΣΣ 4πM 2 G µν G µν [Glashow 86] neutrino-neutrino A A mixing: M llφφ + M l l φ φ + D M ll φφ [Foot and Volkas 95] M-parity: A = A, D = D [Z.B. and Mohapatra 95] active-sterile mixing ( ˆm ν ˆm νν ˆm t νν ˆm ν ) = 1 M ( Av 2 Dvv D t vv A vv if v = v maximal mixing θ νν = 45 If v > v, m ν ζm ν and θ νν ζ 1 ; ζ = v /v 100 ; ζ 10 2 : kev sterile neutrinos (WDM) [Z.B. Dolgov, Mohapatra 96] If A, A = 0 (L L conserved) ) naturally light Dirac neutrinos, DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 10/??

22 See-saw: heavy singlet neutrinos as messengers Introduce heavy gauge singlet fermions N a, a = 1, 2, 3,... with large Majorana mass terms 1 2 (M abn a N b + M abñañb), DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 11/??

23 See-saw: heavy singlet neutrinos as messengers Introduce heavy gauge singlet fermions N a, a = 1, 2, 3,... with large Majorana mass terms 1 2 (M abn a N b + M abñañb), They can equally talk with both O and M leptons y ia l i N a φ + y ia λ i N aφ + M 2 g abn a N b + h.c. ; (y = y ) DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 11/??

24 See-saw: heavy singlet neutrinos as messengers Introduce heavy gauge singlet fermions N a, a = 1, 2, 3,... with large Majorana mass terms 1 2 (M abn a N b + M abñañb), They can equally talk with both O and M leptons y ia l i N a φ + y ia λ i N aφ + M 2 g abn a N b + h.c. ; (y = y ) After decoupling heavy neutrinos, effective operators A A M llφφ + M l l φ φ + D M ll φφ are generated, where A = yg 1 y t, A = y g 1 y t, D = yg 1 y t generate O (active) and M (sterile) neutrino masses and mixings DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 11/??

25 See-saw: heavy singlet neutrinos as messengers Introduce heavy gauge singlet fermions N a, a = 1, 2, 3,... with large Majorana mass terms 1 2 (M abn a N b + M abñañb), They can equally talk with both O and M leptons y ia l i N a φ + y ia λ i N aφ + M 2 g abn a N b + h.c. ; (y = y ) After decoupling heavy neutrinos, effective operators A A M llφφ + M l l φ φ + D M ll φφ are generated, where A = yg 1 y t, A = y g 1 y t, D = yg 1 y t generate O (active) and M (sterile) neutrino masses and mixings They generate also processes like lφ l φ (l φ ) ( L = 1) and lφ l φ ( L = 2), which A. violate L (and so B L) [Sakharov 67] B. violate CP C. should be out-of-equilibrium and thus can generate B-L 0 ( B 0 by sphalerons) DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 11/??

26 See-saw: heavy singlet neutrinos as messengers Introduce heavy gauge singlet fermions N a, a = 1, 2, 3,... with large Majorana mass terms 1 2 (M abn a N b + M abñañb), They can equally talk with both O and M leptons y ia l i N a φ + y ia λ i N aφ + M 2 g abn a N b + h.c. ; (y = y ) After decoupling heavy neutrinos, effective operators A A M llφφ + M l l φ φ + D M ll φφ are generated, where A = yg 1 y t, A = y g 1 y t, D = yg 1 y t generate O (active) and M (sterile) neutrino masses and mixings They generate also processes like lφ l φ (l φ ) ( L = 1) and lφ l φ ( L = 2), which A. violate L (and so B L) [Sakharov 67] B. violate CP C. should be out-of-equilibrium and thus can generate B-L 0 ( B 0 by sphalerons) DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 11/??

27 BBN constraint At the BBN epoch, T 1 MeV, g = g SM = (as contributed by the γ, e ± and 3 ν species) DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 12/??

28 BBN constraint At the BBN epoch, T 1 MeV, g = g SM = (as contributed by the γ, e ± and 3 ν species) Mirror world with T = T would give the same contribution: g = 2 g SM = 21.5 equivalent to N ν = 6.14 DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 12/??

29 BBN constraint At the BBN epoch, T 1 MeV, g = g SM = (as contributed by the γ, e ± and 3 ν species) Mirror world with T = T would give the same contribution: g = 2 g SM = 21.5 equivalent to N ν = 6.14 If T < T, g g SM (1 + x 4 ), equivalent to N ν = 6.14 x 4 x = T /T : E.g. N ν < 0.4 requires x < 0.5; for x = 0.3 N ν < DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 12/??

30 BBN constraint At the BBN epoch, T 1 MeV, g = g SM = (as contributed by the γ, e ± and 3 ν species) Mirror world with T = T would give the same contribution: g = 2 g SM = 21.5 equivalent to N ν = 6.14 If T < T, g g SM (1 + x 4 ), equivalent to N ν = 6.14 x 4 x = T /T : E.g. N ν < 0.4 requires x < 0.5; for x = 0.3 N ν < A paradigm: After inflation O and M worlds are (re)heated in non-symmetric way, T < T The processes between O and M particles are slow enough and are out-of-equilibrium both sectors evolve adiabatically, without significant entropy production, and x = T /T remains nearly constant at later epochs DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 12/??

31 Æ Æ ¼ Ð ¼ ¼ Ð ¼ ¼ Ð ¼ Æ Æ ¼ Ð ¼ ¼ Ð ¼ ¼ Ð ¼ Æ Æ ¼ Ð ¼ Ð Ð Æ ¼ Ð ¼ Ð Ð CP violation in L=1 and L=2 processes Æ Ð Ð Æ Ð Ð Ð Ð Ð Ð Æ Æ Ð Ð Æ Æ Æ Æ Æ Ð Ð Ð Ð [Z.B. and L. Bento 01] DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 13/??

32 Boltzmann Eqs. Evolution for (B-L) and (B-L) T R M dn B L dt + 3Hn B L + Γn B L = 3 4 σ n2 eq dn B L dt + 3Hn B L + Γ n B L = 3 4 σ n 2 eq Γ n eq/m 2 is the effective reaction rate of L = 1 and L = 2 processes Γ /Γ n eq/n eq x 3 ; x = T /T σ = σ = 3ε CP S 32π 2 M 4 where S 16T 2 is the c.m. energy square, ε CP = ImTr[(y y) g 1 (y y )g 2 (y y)g 1 ] Y BL = D(k) Y (0) BL ; Y BL = D(kx3 ) Y (0) BL Y (0) BL ε CP M P l T 3 R g 3/2 M 4. DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 14/??

33 Exact M-parity: M N = M N n B /n B = D(k), k = [Γ eff/h] T=TR : Ω B /Ω B Depletion factor D(k) = 3 5 e k F(k) G(k); for k 1, D(k) = 1 [ F(k) = 1 4k (2k 1) 3 + 6k 5 + 6e 2k] : T > T 4 R, [ G(k) = 3 k 2 (k 2 + 2k + 2)e k] ; T < T 3 R Heating: N ν k/g x = (k/6g ) 1/4 < 0.2: k 2, (LSS) DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 15/??

34 Broken M parity: M W > M W? Spont. broken M parity: v v [Z.B., Dolgov & Mohapatra 96] Α3 1 Μ Α 3 Α SUSY n B n B Μ GeV k < 1 (robust non-equilibrium) M N /M N (Λ /Λ) changes slowly with M W m e/m e M W /M W changes fastly with M W. Properties of MB s get closer to CDM : M W 10 TeV? DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 16/??

35 Mirror Matter Evolution epochs [Z.B., Comelli & Villante, 01] Earlier decoupling of mirror photons (x < 0.5): z dec x 1 z dec x eq = 0.05(Ω M h 2 ) Jeans scale is smaller : λ J d H before Matter=Radiation Silk scale is smaller : λ S 5x5/4 eq (x/x eq ) 3/2 (Ω M h 2 ) 3/4 Mpc DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 17/??

36 CMB & LSS power spectra [l(l+1)c l /2π] 1/2 (µκ) Ω M =0.25, ω b =0.023, h=0.73, n=0.97 x=0.5, no CDM x=0.3, no CDM x=0.2, no CDM 20 WMAP ACBAR l 2df bin. P(k)h 3 (Mpc 3 ) k/h (Mpc 1 ) DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 18/??

37 LSS power spectra [Z.B., Ciarcelluti, Comelli & Villante, 03] P(k)h 3 (Mpc 3 ) Ω M =0.30,ω b =0.001,h=0.70,n=1.00 Ω M =0.30,ω b =0.02,h=0.70,n=1.00 Ω M =0.30,ω b =0.02,h=0.70,x=0.2,no CDM,n=1.00 Ω M =0.30,ω b =0.02,h=0.70,x=0.1,no CDM,n=1.00 Ω M =0.30,ω b =0.02,h=0.70,x=0.2,ω b =ω CDM,n= k/h (Mpc 1 ) DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 19/??

38 Neutron - Mirror neutron mixing Baryogenesis via L- or via B-breaking [Z.B. and L. Bento 06] d 1 d φ S u N l M N M φ l N N S d u d M (udd)(u d d ) M (qqd)(q q d ) + h.c. δm (nn + n n) 5 δm ( ) 10 TeV 5 M ev!! τ osc 1 sec!! but τ dec 10 3 sec?? P(t) = e t/τ dec P(t) = cos 2 (t/τ osc ) e t/τ dec 1 2 e t/τ dec?? DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 20/??

39 Neutron - Mirror neutron oscillation Effective (non-relativistic) Hamiltonian for n n oscillation ( ) p 2 /2m iγ n /2 V δm H = δm p 2 /2m iγ n /2 V The mass m and decay width Γ n = 1/τ dec due to exact mirror parity, are precisely the same for the neutrons and mirror neutrons! But the potentials V and V are not the same - V V 0! V = 0 on the Earth, but V µb ev (B 0.5 G Earth magnetic field, µ neutron magnetic moment) In vacuum τ osc = τ = δm 1, θ mix = 45 : P(t) = cos 2 (t/τ) e t/τ dec 1 2 e t/τ dec In medium τ eff = τ/ 1 + (µb/2δm) 2 : for µb δm, τ eff (µb/2) 1 sin2θ eff = τ eff δm = τ eff /τ: for µb δm, sin2θ eff (2δm/µB) Transition probab. P nn (t) = 1 P(t) = (τ eff /τ) 2 sin 2 (t/τ eff ) e t/τ dec, For t τ eff, P nn (t) (t/τ) 2 DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 21/??

40 Experimental limits & and future search Grenoble experiment for neutron - antineutron oscillation search: 100 m long mumetal tube, B < 10 4 G, t 0.1 s no n ñ event found : τ nñ > 10 8 s (or > 3yr) about 5% neutron deficit was observed, P nn (t) (t/τ) 2 < 0.5 : τ > 0.5 sec Important!! n ñ destabilizes nuclei: (A, Z) (A 1, Z, ñ) (A 2, Z) + π s n n oscillation cannot destabilize nuclei: (A, Z) (A 1, Z) + n not allowed!!!! δm 1 = τ 1 sec is allowed!!!. Implications Anomalous Neutron Loses, Lifetime measurements, UHECR,... DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 22/??

41 Mirror Physics & Cosmology: Summary String Theory: parallel D-branes or brane-antibrane restoring Parity: L R can remain exact (models of exact mirror parity) or spontaneously broken (ZB, Dolgov & Mohapatra) Common gauge forces between two sectors: e.g. U(1) B L, or (anomaly free) gauge flavour symmetry SU(3) H between fermion families: helps for SUSY flavour changing problem (safe D-terms) ZB 1998 Higgs sector stability: Higgs as pseudogoldstone in SUSY accidental global U(4) symmetry (ZB 2005, Falkowski, Pokorski, Schmalz 06) Photon - photon kynetic mixing (invisible 0-Ps decay) neutrino - neutrino (active - sterile) mixing neutron - neutron mixing (hydrogen - hydrogen ) mixing pion - pion mixing (DAMA vs. CDMS) Kaon - Kaon mixing (new features in CP-violation?) etc. etc. Strong CP-problem: new models for axion avoiding mass-coupling correlation m a f π m pi /f a (ZB, Gianfagna, Gianotti 2000) DOLGOV FEST, XI Gran Sasso Summer Institute, June 28, 2007 Mirror World:... - p. 23/??

arxiv:astro-ph/ v1 28 Apr 2005 MIRROR WORLD AND AXION: RELAXING COSMOLOGICAL BOUNDS

arxiv:astro-ph/ v1 28 Apr 2005 MIRROR WORLD AND AXION: RELAXING COSMOLOGICAL BOUNDS International Journal of Modern Physics A c World Scientific Publishing Company arxiv:astro-ph/0504636v1 28 Apr 2005 MIRROR WORLD AND AXION: RELAXING COSMOLOGICAL BOUNDS MAURIZIO GIANNOTTI Dipartimento