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High energy neutrino astronomy: Challenges & Prospects

High energy neutrino astronomy: Challenges & Prospects. Eli Waxman Weizmann Institute, ISRAEL. High energy n ’ s: A new window. MeV n detectors: Solar & SN1987A n ’ s Stellar physics (Sun ’ s core, SNe core collapse) n physics >0.1 TeV n detectors:

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High energy neutrino astronomy: Challenges & Prospects

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  1. High energy neutrino astronomy:Challenges & Prospects Eli Waxman Weizmann Institute, ISRAEL

  2. High energy n’s: A new window MeV n detectors: • Solar & SN1987A n’s • Stellar physics (Sun’s core, SNe core collapse) • n physics >0.1 TeV n detectors: • Extendn horizon to extra-Galactic scale MeV n detectors limited to local (Galactic) sources [10kt @ 1MeV1Gton @ TeV , sTeV/sMeV~106] • Study “Cosmic accelerators” [pg, pp  p’sn’s] • n physics

  3. HEN detector motivation:Cosmic accelerators log [dJ/dE] E-2.7 Galactic Protons E-3 Source: Supernovae(?) X-Galactic (?) Heavy Nuclei Source? Light Nuclei? Lighter Source? 1 1010 106 Cosmic-ray E [GeV] [Blandford & Eichler, Phys. Rep. 87; Axford, ApJS 94; Nagano & Watson, Rev. Mod. Phys. 00]

  4. UHE, >1010GeV, CRs J(>1011GeV)~1 / 100 km2 year 2p sr Auger: 3000 km2 3,000 km2 Fluorescence detector Ground array

  5. Composition clues Auger 2009 HiRes 2005

  6. Flux & Spectrum • E2(dN/dE)=E2(dQ/dE) teff. (teff. : p + gCMB N +p) • Assume: p, dQ/dE~(1+z)mE-a cteff [Mpc] log(E2dQ/dE) [erg/Mpc2 yr] GZK (CMB) suppression • >1019.3eV: consistent with • protons, E2(dQ/dE) ~1043.7 erg/Mpc3 yr + GZK • E2(dQ/dE) ~Const.: Consistent with shock acceleration [Katz & Waxman 09] [Waxman 1995; Bahcall & Waxman 03] [Krimsky 77; Bednarz & Ostrowski 98; Keshet & Waxman 05 cf. Lemoine & Revenu 06]

  7. Anisotropy clues Biased (rsource~rgal for rgal>rgal ) CR intensity map (rsource~rgal) Galaxy density integrated to 75Mpc • Cross-correlation signal: Anisotropy @ 98% CL; Consistent with LSS • Correlation with AGN ? VCV catalogue: Anisotropy @ 99% CL  low-luminosity AGN? Simply trace LSS! (& VCV non-uniform, incomplete…) [Kashti & Waxman 08] [Waxman, Fisher & Piran 1997] [Auger collaboration 07]

  8. Composition-Anisotropy connection • Plausible assumptions: Acceleration of Z(>>1) to E ~ Acceleration of p to E/Z Jp(E/Z)>=JZ(E/Z) + Note: p(E/Z) propagation = Z(E) propagation  Anisotropy of Z at 1019.7eV implies Stronger aniso. signal (due to p) at (1019.7/Z) eV ! Not observed! [:Lemoine & Waxman 09]

  9. The 1020eV challenge v R B /G v G2 G2 2R l =R/G (dtRF=R/Gc) [Waxman 95, 04, Norman et al. 95]

  10. Suspects • - L>1012 (G2/b) Lsun: • * Extra-Galactic • * Non at d<dGZK  Transient • - E2(dQ/dE) ~1043.7 erg/Mpc3 yr • Gamma-ray Bursts (GRBs) • G~ 102.5, Lg~ 1019LSun L/G2 >1012 Lsun • (dn/dVdt)*E~10-9.5 /Mpc3 yr *1053.5erg • ~1044 erg/Mpc3 yr • Transient: DTg~10s << DTpg ~105 yr • Active Galactic Nuclei (AGN, Steady): • G~ 101 L>1014 LSun=few brightest • !! Non at d<dGZK  Invoke: • “Dark” (proton only) AGN • L~ 1014 LSun , Dt~1month flares from • stellar disruptions [Waxman 95, Vietri 95, Milgrom & Usov 95] [Waxman 95] [Blandford 76; Lovelace 76] [Boldt & Loewenstein 00] [Farrar & Gruzinov 08]

  11. Source physics challenges • GRB: 1020LSun, MBH~1Msun, M~1Msun/s, G~102.5 • AGN: 1014 LSun, MBH~109Msun, M~1Msun/yr, G~101 • MQ: 105 LSun, MBH~1Msun, M~10-8Msun/yr, G~100.5 Jet acceleration [Reviws: GRBs Kouveliotou 94; Piran 05 AGN Begelman, Blandford & Rees 84 MQ HE: Aharonian et al 2005; Khangulyan et al 2007] Energy extraction Particle acceleration Jet content (kinetic/Poynting) Radiation mechanisms

  12. Cosmic accelerators: clues & open Q’s • X-Galactic, (?)protons “Conventional” accelerators Ep2dN/dEp~ 0.6x1044 erg/Mpc3 yr • Open Q’s: Primaries Source identity Acceleration process Cosmic-accelerators physics (BH accretion jets, Baryonic/EM…)

  13. HE n Astronomy • p + g N +p p0 2g ; p+  e+ + ne + nm + nm  Identify UHECR sources Study BH accretion/acceleration physics • E2dn/dE=1044erg/Mpc3yr & tgp<1: • If X-G p’s:  Identify primaries, determine f(z) [Waxman & Bahcall 99; Bahcall & Waxman 01] [Berezinsky & Zatsepin 69]

  14. HE n experiments Optical Cerenkov - South Pole Amanda: 660 OM, 0.05 km3 IceCube: +660/yr OM (05/06…) 4800 OM=1 km3s - Mediterranean Antares: 10 lines (Nov 07), 750 OM 0.05 km3 Nestor: (?)  0.1 km3 km3Net: R&D  1 km3 • UHE: Radio Air shower • Aura, Ariana (in Ice) Auger (nt) • ANITA (Balloon) EUSO (?) • LOFAR

  15. Single flavor Multi flavor [Anchordoqui & Montaruli 09]

  16. Star bursts: A lower bound? • Star burst galaxies: - Star Formation Rate ~103Msun/yr >> 1 Msun/yr “normal” (MW) - Density ~103/cc >> 1/cc “normal” - B ~1 mG >> 1mG “normal” • Most stars formed in (z>1.5) star bursts • High density + B: CR e-’s lose all energy to synchrotron radiation CR p’s lose all energy to p production [Quataert et al. 06] [Loeb & Waxman 06]

  17. M82 M81 Mark Westmoquette (University College London), Jay Gallagher (University of Wisconsin-Madison), Linda Smith (University College London), WIYN//NSF, NASA/ESA Robert Gendler

  18. Starbursts Synchrotron radio Fn calibration p0gg, Fn ~Fg M82, NGC253: Hess, VERITAS 09 Fermi 09 dN/dE~1/Ep, p<~2.2 [Loeb & Waxman 06]

  19. GRB n’s • If: Baryonic jet • Background free: [Waxman & Bahcall 97, 99; Rachen & Meszaros 98; Alvarez-Muniz & F. Halzen 99; Guetta et al. 04; Hooper, Alvarez-Muniz, Halzen & E. Reuveni 04]

  20. The current limit [Achterberg et al. 08 (The IceCube collaboration)]

  21. n- physics & astro-physics [Waxman & Bahcall 97] • p decay  ne:nm:nt = 1:2:0 (Osc.) ne:nm:nt = 1:1:1 t appearance experiment • GRBs: n-g timing (10s over Hubble distance) LI to 1:1016; WEP to 1:106 • EM energy loss of m’s (and p’s) • ne:nm:nt = 1:1:1 (E>E0) 1:2:2 • GRBs: E0~1015eV • Combining E<E0, E>E0 flavor measurements may constrain CPV [SinQ13 Cosd] [Waxman & Bahcall 97; Amelino-Camelia,et al.98; Coleman &.Glashow 99; Jacob & Piran 07] [Rachen & Meszaros 98; Kashti & Waxman 05] [Blum, Nir & Waxman 05]

  22. Outlook • Particle+Astro-phys. Open Q’s - >1011GeV particles: primaries, f(z),origin & acceleration - Physics of relativistic sources (GRBs, AGN, MQ…) - <1011GeV particles: sources, acceleration, propagation (SNRs, starbursts, …) - nm ntt appearance gn Timing  LI to 1:1016; WEP to 1:106 Flavor ratios  CPV • New HE g, CR and n detectors >103 km2 hybrid >1019eV CR detectors ~1 km3 (=1Gton) 1-1000TeV n detectors >>1 km3[radio,…] >>1000TeV n detectors 10MeV—10GeV g-ray satellite (AGILE, GLAST) >0.1TeV (ground based) g-ray telescopes (Milagro, HESS, MAGIC, VERITAS) Point sources

  23. & IceCube AMANDA

  24. The Mediterranean effort • ANTARES (NESTOR, NEMO) KM3NeT

  25. Back up slides

  26. Electrons MeV g’s: tgg<1: e- (g) spectrum: e- (g)energy production Protons Acceleration/expansion: Synchrotron losses: Proton spectrum: p energy production: GRB proton/electron acceleration 52 Afterglow, RGRB~SFR [Waxman 95, 04]

  27. The GRB “GZK sphere” g p • LSS filaments: D~1Mpc, fV~0.1, n~10-6cm-3, T~0.1keV eB=(B2/8p)/nT~0.01 (B~0.01mG), lB~10kpc • Prediction: D lB [Waxman 95; Miralda-Escude & Waxman 96, Waxman 04]

  28. GRB Model Predictions [Miralda-Escude & Waxman 96]

  29. AGN n models?? BBR05

  30. >1019eV cosmic rays: Clue summary • Spectrum (+Xmax)  likely X-Galactic protons • Anisotropy + Spectrum  likely “Conventional” sources • L constraint  likely Transient sources • Ep2dN/dEp~ 0.7x1044 erg/Mpc3 yr • What next for Auger? Identify (narrow spectrum) point source(s)?

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