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Neutrino (Mass) in Cosmology

Neutrino (Mass) in Cosmology. Thomas J. Weiler Vanderbilt University Nashville TN 37235, and CERN, Geneva, Switzerland. Early-Universe Timeline. Friedmann eqns, and energy partitions Omega. with “a” being the cosmic scale factor. So L behaves like a “matter” with 3p+ r < 0 !.

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Neutrino (Mass) in Cosmology

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  1. Neutrino (Mass) in Cosmology Thomas J. Weiler Vanderbilt University Nashville TN 37235, and CERN, Geneva, Switzerland Thomas J. Weiler, Vanderbilt University & CERN

  2. Early-Universe Timeline Thomas J. Weiler, Vanderbilt University & CERN

  3. Friedmann eqns, and energy partitions Omega with “a” being the cosmic scale factor So L behaves like a “matter” with 3p+r < 0 ! Can relate (F1) parameters to today’s values to write Omega=r/rcrit, rcrit=6 protons/m3 Inflation and data  OmegaK ~ 0 Thomas J. Weiler, Vanderbilt University & CERN

  4. Neutrino Decoupling Looking back, n’s last scattered at time t such that i.e. GF2 T5 ~ T2/MP , TnDC ~ MeV, t ~ 1 s, z ~ 1010. Coincidentally, TnDC ~ TBBN ~ Te+e- vs. zeq = a0/aeq = Omegarad/Omegam ~ 4000, zrecomb ~ 1100. Coincidentally, Teq~ Trecomb ~ eV ~ mn Thomas J. Weiler, Vanderbilt University & CERN

  5. Neutrino stat mech per flavor HDM models tried (top-down) Omegan=1, i.e. each mn~30eV Thomas J. Weiler, Vanderbilt University & CERN

  6. Neutrino density from BB photon density Thomas J. Weiler, Vanderbilt University & CERN

  7. nn, ng >> any other density SN87a sun Neutrino Incognito ~CnB hadron wall? no wall a’tall Thomas J. Weiler, Vanderbilt University & CERN

  8. Neutrino time Liberated at T=Mev, t= 1 sec Depends on energy (Lorentz boost) Consider a 1020 eV neutrino. Lorentz factor = 1021 for mn = 0.1 eV. Age of Uni is 1018 sec, But age of n is 1018/1021 sec = 1 millisecond ! And it doesn’t even see the stream of radiation rushing past it – untouched ! Thomas J. Weiler, Vanderbilt University & CERN

  9. CR Spectrum above a TeV from Tom Gaisser 50 Joules VLHC (100 TeV)2 Thomas J. Weiler, Vanderbilt University & CERN

  10. BBN limits on Nnand asymmetry • Competing effects: • Weak int’n rate equilibrates ne+n  p+e- , as n/p ~ exp[-dmN/TnDC] ; • So more ne  less neutrons  less He/H • Expansion rate (monotonic with Nn) decouples weak int’n; • So more Nn faster movie, earlier hotter TnDC and more neutrons  more He/H Kneller & Steigman H S H, S = So one extra species is DS=0.08 Best fit is DN=0.25, L=2.5% Thomas J. Weiler, Vanderbilt University & CERN

  11. Compensation and LSND Order 5% neutrino asymmetry -- to be contrasted with 10-9 baryon asymmetry Thomas J. Weiler, Vanderbilt University & CERN

  12. Four roads to absolute neutrino mass(SN discounted) • 1. Tritium decay • 2. 0vbb decay • 3. WMAP  LSS • 4. Z-bursts on the relic CnB Thomas J. Weiler, Vanderbilt University & CERN

  13. Tritium decay limits on neutrino mass Q: Why tritium? A: It has a small Q-value, mT-(mD+mp+me) Thomas J. Weiler, Vanderbilt University & CERN

  14. The oscillation “box” from a Feynman graph Where does the “mixing matrix” come in? Thomas J. Weiler, Vanderbilt University & CERN

  15. PMNS neutrino-mixing matrix Weak-interaction and mass “vectors” point differently: |nk>=Uki |ni>, or Uki = <ni | nk> = <nk | ni>* Thomas J. Weiler, Vanderbilt University & CERN

  16. It “probably” looks something like this m3 Dm223 ~ 2.5 x 10-3 eV2 m2 Dm212 ~ 7 x 10-5 eV2 m1 nm ne nt What we think we know about neutrino mass Log m2 Thomas J. Weiler, Vanderbilt University & CERN

  17. m3 m3 m2 m2 m1 m1 nm ne nt Or maybe … It looks like this Log m2 Thomas J. Weiler, Vanderbilt University & CERN

  18. Naturalness may be over-rated Do these look natural? A rodent with a bill? Or a bug with a light-emitting tush? Thomas J. Weiler, Vanderbilt University & CERN

  19. 0nbb decay limits on neutrino mass Thomas J. Weiler, Vanderbilt University & CERN

  20. Neutrino parameters: fundamental to physics, and a tool for astrophysics/cosmology As an astro tool, useful NOW (e.g. Le = Lm = Lt ) ; As a physics window, the view is unclear. Thomas J. Weiler, Vanderbilt University & CERN

  21. neutrino masses and cosmology r [% of rcr] first task: bound n mass second task: decide whether n contribute as Hot Dark Matter Thomas J. Weiler, Vanderbilt University & CERN

  22. Cosmic structure formation WMAP  2dF/SDSS * Thomas J. Weiler, Vanderbilt University & CERN

  23. COBE data • *The raw temperature map (top) has a large diagonal asymmetry due to our motion with respect to the cosmic microwave background • a Doppler shift. • *The temperature fluctuations after subtraction of the velocity contribution, • showing primordial fluctuations and a large radio signal from nearby sources in our own galaxy (the horizontal strip). • *The primordial fluctuations after subtraction of the galaxy signal. V Thomas J. Weiler, Vanderbilt University & CERN

  24. WMAP data The Universe at trecombination , ~ tequality Thomas J. Weiler, Vanderbilt University & CERN

  25. 2dF Galaxy Redshift Survey Peak from horizon scale at teq HDM contributes to suppression of Small scales Thomas J. Weiler, Vanderbilt University & CERN

  26. New length scale from neutrino mass LSS formation is a battle between attractive gravity and repulsive pressure; the battle-line is the “Jean’s length” (4pGr/vs2)1/2 ~ (4pG/p)1/2 . The knr ~ (Omegan/Omegam)1/2 Omegam WMAP LSS Today k > Thomas J. Weiler, Vanderbilt University & CERN

  27. Tegmark cosmic cinema - CDM http://www.hep.upenn.edu/~max/cmb/movies.html Increasing the total density of matter (baryons + cold dark matter) pushes the epoch of matter-radiation equality back in time and moves the peak scale (the horizion size at that time) to the right. Thomas J. Weiler, Vanderbilt University & CERN

  28. Tegmark cosmic cinema - HDM Increasing the density of massive neutrinos suppresses all scales smaller than a certain cutoff, which in turn shifts to the left as you increase the neutrino mass (and density) Thomas J. Weiler, Vanderbilt University & CERN

  29. Tegmark cosmic cinema – more HDM If a CMB theorist gloats that he or she can measure the neutrino density, make sure to point out that galaxy surveys are much more sensitive. Thomas J. Weiler, Vanderbilt University & CERN

  30. A little HDM history Thomas J. Weiler, Vanderbilt University & CERN

  31. Neutrino fits Elgaroy and Lahav Thomas J. Weiler, Vanderbilt University & CERN

  32. SDSS (Seljak et al) Increasing nu mass increases CMB spectrum, But decreases matter power spectrum ?? Thomas J. Weiler, Vanderbilt University & CERN

  33. Role of priors (Elgaroy and Kahav) Elgaroy and Lahav Thomas J. Weiler, Vanderbilt University & CERN

  34. Resonant Neutrino Annihilation Mean-Free-Path l=(nn sn)-1 = 40 DH/h70 Fig: Fargion, Mele, Salis Thomas J. Weiler, Vanderbilt University & CERN

  35. Escher’s “Angels and Devils” The early Uni was denser, more absorbing. Thomas J. Weiler, Vanderbilt University & CERN

  36. Neutrino mass-spectroscopy: absorption and emission Thomas J. Weiler, Vanderbilt University & CERN

  37. Z-bursts TJW, 1982; Revival – 1997 ~ 50 Mpc Thomas J. Weiler, Vanderbilt University & CERN

  38. n-mass spectroscopy zmax=2, 5, 20 (top to bottom), n-a=2 (bottom-up acceleration) Eberle, Ringwald, Song, TJW, 2004 Thomas J. Weiler, Vanderbilt University & CERN

  39. Dips & sobering realism • hidden MX=4 1014 and 1016 GeV, • to explain >GZK w/ Z-bursts; • mass = 0.2 (0.4) eV - dashed (solid); Error bars – per energy decade, by 2013, for flux saturating present limits Thomas J. Weiler, Vanderbilt University & CERN

  40. The GZK puzzle Thomas J. Weiler, Vanderbilt University & CERN

  41. Z-burst spectrum Thomas J. Weiler, Vanderbilt University & CERN

  42. Fitted Z-burst (Emission) Flux Gelmini, Varieschi, TJW Thomas J. Weiler, Vanderbilt University & CERN

  43. Nu-mass limit for Z-burst fitted to EECRs Gelmini, Varieschi, TJW Thomas J. Weiler, Vanderbilt University & CERN

  44. Size matters EUSO ~ 300 x AGASA ~ 10 x Auger EUSO (Instantaneous) ~3000 x AGASA ~ 100 x Auger Thomas J. Weiler, Vanderbilt University & CERN

  45. “clear moonless nights” Thomas J. Weiler, Vanderbilt University & CERN

  46. See-saw (Leptogenesis to follow) Thomas J. Weiler, Vanderbilt University & CERN

  47. Leptogenesis • Three Sakharov conditions for Violate baryon number (B-L conserved => Baryogenesis: • DB (=DL) nonzero • Violate C and CP  T (complex couplings) • Out of Thermal Equilibrium • (decouple at T > M so no Boltzmann suppression, • then decay at T < M when over-abundant) Thomas J. Weiler, Vanderbilt University & CERN

  48. Extra-dimensions and neutrino mass Right-handed “sterile” neutrinos may be our probe of extra-dimensions Thomas J. Weiler, Vanderbilt University & CERN

  49. Summary: Neutrinos are a splendid example of the interplay among particle physics, astrophysics, and cosmology Thomas J. Weiler, Vanderbilt University & CERN

  50. Thomas J. Weiler, Vanderbilt University & CERN

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