Astrophysics of high energy cosmicrays

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Astrophysics of high energy cosmic-rays

• Eli Waxman
• Weizmann Institute, ISRAEL

New Physics talk by M. Drees
Bhattacharjee Sigl 2000
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Cosmic ray flux and Composition
log dJ/dE
E-2.7
Galactic
Protons
E-3
X-Galactic
Heavy Nuclei
Galactic plane enhancement
Light Nuclei (p?)
Isotropy
1
106
1010
E GeV
Ucr(1GeV)1 eV/cm3
Blandford Eichler, Phys. Rep. 87 Axford, ApJS
94 Nagano Watson, Rev. Mod. Phys. 00
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Challenge I Acceleration
v
R
B
v
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Brightest known sources

• AGN jets (steady)
• G few requires L1047 erg/s
• Few, brightest AGN
• GRBs (transient)
• G 300 requires L1051 erg/s
• Average Lg1052 erg/s

Srittmatter 82 Biermann Strittmatter 87
Waxman 95 Vietri 95 Milgrom Usov 95
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The Suspects
losses
1/b
Hillas 84 Arisaka 02
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Comments on Magnetars

• Newborn Neutron stars
• (Hypothesis) with B1014G, W104/sec
• LEM1050
  erg/s for t
• Some difficulties
• Wind should penetrate envelope
• with
• Acceleration mechanism
  Unknown

e.g. Blasi, Epstein, Olinto 00 Arons 02
EM wind
NS
1 Msun envelope
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Challenge II Propagation (GZK)
g
p(p0)
CMB
n (p)
p
1000
100
10
0.5
1.0
3.0
Greisen 66 Zatsepin Kuzmin 66
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Model
Waxman 95

• Flys Eye fit for Galactic heavy (
• JGE-3.50
• X-Galactic protons
• Generation spectrum (shock
  acceleration)
• Generation rate (GRB motivated)
• Redshift evolution SFR (GRB
  motivated).

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The Data
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Data- Calibrated at 1019eV
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Model vs. Data
Bahcall Waxman 02
X-G Model
Ruled out 7s
5s
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Conclusions are Robust
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Data/Model consistency

• Yakutsk, Flys Eye, HiRes Consistent with
• XG protons
  GZK
• AGASA (25 of total exposure)
• Consistent below 1020eV
• Excess above 1020eV 2.2/-0.8 8
  observed
• New source/New physics/ 25 energy
  
• Local inhomogeneity
  over-estimate
• Need Large, hybrid 1018eV to 1020eV detector
  (Auger)

?
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The Auger Observatory 103.5 km2
Cronin 92, Watson 93
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Gamma-ray Bursts
M on 1 Solar Mass BH
Relativistic Outflow
G300
e- acceleration in Collisionless shocks
e- Synchrotron MeV gs Lg1052erg/s
Meszaros, ARAA 02
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Proton/electron acceleration
Waxman 95

• Protons
• Acceleration
• Particle spectrum
• p energy production

• Electrons
• MeV gs
• g spectrum
• g energy production

Frail et al. 01 Schmidt 01
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GZK Sources

• AGN, Radio-galaxies ?
• GRBs ?
• For RGRB(z0)0.5/Gpc3yr
• Prediction

g
Waxman 95, 01
p
Schmidt 01
D
lB
Miralda-Escude Waxman 96
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GRBs An illustrative example
Miralda-Escude Waxman 96
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GRB Model Predictions

• Homogeneous GZK
• 3x1020eV
• Few, narrow spectrum sources
• Fluctuations (no homogeneous GZK)
• For more
• Lec. Notes Phys. review
  (astro-ph/0103186)

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Standard Model GRB ns

• Weak dependence on model parameters

Waxman Bahcall 97, 99
Rachen Meszaros 98 Guetta, Spada Waxman 01
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Diffuse n Flux Bound

• Observed JCR(1019eV)
• pg losses on CMB z
• For Sources with tgp
• Strongest know z evolution (QSO, SFR)

Waxman Bahcall 99, Bahcall Waxman 01
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tgp for known sources
eg
p
e
n
e-
eg
ep
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Anita (Radio, Balloon)
Antares (0.1 Gton)
Nemo (1 Gton)
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The AMANDA South-pole experiment
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AMANDA neutrino event
Andres et al., Nature 01
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The Mediterranean ANTARES experiment
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Summary

• Yakutsk, Flys Eye, HiRes Consistent with GZK
• AGASA 1020eV excess
• Main Challenge Astrophysical accelerator
  physics
• Candidate GRBs
• Hybrid, 103.5km2 Auger
• GZK spectrum Constraints on astro.
  sources
• UHE CRs High energy n sources
• 1--103TeV 1 km3 (Optical Cerenkov)
  detectors
• Amanda, Antares,
  Nestor, IceCube, Nemo
• 103TeV 1 km3 (Radio Cerenkov)
  detectors
• Anita, Rice

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n telescopes some prospects

• GRB n detection
• nm nt t appearance
• Lorentz Inv. (1-v/c 10-16),
• Weak equivalence principle
  (FL/c3 10-6)