High Energy CosmicRays and High Energy Neutrino Astronomy

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High Energy Cosmic-Rays and High Energy Neutrino
Astronomy

• Eli Waxman, Weizmann Inst., Israel

Tribute to John N. Bahcall Neutrino
Oscillations in Venice, Feb. 06
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High energy ns A new window

• MeV n detectors
• Solar SN1987A ns
• Stellar physics (Suns core, SNe core collapse)
• n physics
• gt0.1 TeV n detectors
• Extend n horizon to extra-Galactic scale
• MeV n detectors limited to local (Galactic)
  sources
• 10kt _at_ 1MeV?1Gton _at_ TeV , sTeV/sMeV106
• Study Cosmic accelerators pg, pp ? ps?ns
• n physics

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What do we know aboutXG cosmic accelerators?

• They exist
• gt1020 eV cosmic-rays detected
• gt1019 eV Isotropic
• Extra-Galactic (light?) nuclei

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Open Qs I. Acceleration sources
Hillas 1984 Waxman 04

• The suspects
• Active Galactic Nuclei (steady)
• G 101 ? Lgt1014 LSun Few,
  brightest AGN
• Gamma Ray Burstss (transient)
• G 102.5 ? Lgt1017 LSun Lg 1018LSun

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Open Qs II. Source physics

• GRB MBH1Msun, M1Msun/s, G102.5
• AGN MBH109Msun, M1Msun/yr, G101

Jet acceleration
Energy extraction
Particle acceleration
Jet content (kinetic/Poynting)
Radiation mechanisms
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Open Qs III. Spectrum

• J(1020eV)1/100 km2 yr

• Ep gt0.6x1020eV p gCMB ? N p
• dGZK50 Mpc ltlt dH4
  Gpc

Bahcall Waxman 03
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Cosmic variance
Bahcall Waxman 00
GRBs
Miralda-Escude Waxman 96
Waxman 95
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The Auger observatory Hybrid 103.5 km2
Watson 91, Cronin 93
Auger South Argentina (North
Colorado?)

• 1/2 built
• 1,500 km2 yr sr
• 50 syst. energy uncertainty
• Preliminary results
• 1 event gt1020eV (yes GZK)

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n Astronomy a flux bound

• p g ? N p
• p0 ? 2g p ? e ne nm nm
• If p energy converted to p
• For Sources with tgplt1

Waxman Bahcall 99 Bahcall Waxman 01
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Waxman Bahcall 99 Bahcall Waxman 01
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Flux bound Detector size

• Optical Cerenkov
• 0.1 km2 Amanda,
• Antares, Nestor
• 1 km2 IceCube,
• km3Net (NEMO)
• Radio
• Rice, ANITA
• Air shower
• Auger (nt), EUSO

GRBs
Waxman Bahcall 97
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AMANDA
IceCube
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The Mediterranean effort

• ANTARES, NESTOR, NEMO ? km3net

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Outlook

• Cosmic accelerators challenges
• Primaries, sources
• Acceleration
• Physics of extreme sources (GRBs,
  AGN)
• New HE (g,) CR and n detectors
• gt103 km2 hybrid gt1019eV CR
  detectors
• 1 km3 (1Gton) 1-1000TeV n detectors
• gtgt1 km3 radio, gtgt1000TeV n detectors
• n properties with n telescopes
• nm nt ? t appearance
• GRBs lt 10s gn Timing ? LI to 11016 WEP
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