High Energy Cosmic-Rays and High Energy Neutrino Astronomy

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

High energy n’s: A new window Me. V n detectors: • Solar & SN 1987 A n’s • Stellar physics (Sun’s core, SNe core collapse) • n physics >0. 1 Te. V n detectors: • “Extend n horizon to extra-Galactic scale” Me. V n detectors limited to local (Galactic) sources [10 kt @ 1 Me. V 1 Gton @ Te. V , s. Te. V/s. Me. V~106 ] • Study “Cosmic accelerators” [pg, pp p’s n’s] • n physics

What do we know about XG cosmic accelerators? • They exist >1020 e. V cosmic-rays detected >1019 e. V: Isotropic Extra-Galactic (light? ) nuclei

Open Q’s: I. Acceleration & sources [Hillas 1984; Waxman 04] • The suspects: Active Galactic Nuclei (steady): G~ 101 L>1014 LSun: Few, brightest AGN Gamma Ray Burstss (transient): G~ 102. 5 L>1017 LSun : Lg~ 1018 LSun

Open Q’s: II. Source physics • GRB: AGN: MBH~1 Msun, M~1 Msun/s, G~102. 5 MBH~109 Msun, M~1 Msun/yr, G~101 Jet acceleration Energy extraction Jet content (kinetic/Poynting) Particle acceleration Radiation mechanisms

Open Q’s: III. Spectrum • J(1020 e. V)~1/100 km 2 yr • Ep >0. 6 x 1020 e. V: p + g. CMB N + p d. GZK~50 Mpc << d. H~4 Gpc [Bahcall & Waxman 03]

“Cosmic variance” [Bahcall & Waxman 00] GRBs [Miralda-Escude & Waxman 96] [Waxman 95]

The Auger observatory: Hybrid 103. 5 km 2 Auger South: Argentina • • (North: Colorado? ) ~1/2 built ~1, 500 km 2 yr sr ~50% syst. energy uncertainty Preliminary results: ~1 event >1020 e. V (yes GZK) [Watson 91, Cronin 93]

n Astronomy: a flux bound • p+g N+p p 0 2 g ; p+ e+ + ne + nm • If p energy converted to p • For Sources with tgp<1: [Waxman & Bahcall 99; Bahcall & Waxman 01]

[Waxman & Bahcall 99; Bahcall & Waxman 01]

Flux bound & Detector size • Optical Cerenkov 0. 1 km 2: Amanda, Antares, Nestor 1 km 2: Ice. Cube, km 3 Net (NEMO) • Radio Rice, ANITA • Air shower Auger (nt), EUSO GRBs [Waxman & Bahcall 97]

AMANDA & Ice. Cube

The Mediterranean effort • ANTARES, NESTOR, NEMO km 3 net

Outlook • Cosmic accelerators’ challenges Primaries, sources Acceleration Physics of “extreme” sources (GRBs, AGN) • New HE (g, ) CR and n detectors >103 km 2 hybrid >1019 e. V CR detectors ~1 km 3 (=1 Gton) 1 -1000 Te. V n detectors >>1 km 3 [radio, …] >>1000 Te. V n detectors • n properties with n telescopes nm nt t appearance GRBs: < 10 s gn Timing LI to 1: 1016; WEP to 1: 106