Nuclear Burning

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Why Does the Sun Shine?

• Sun Ball of H gas compressed by gravity ? HEAT
  (not enough)
• HEAT ? Nuclear fusion
• p p ? d e n energy

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Solar Properties
L 3.8 x 1026 W 2.4 x 1039 MeV/s M 2 x 1030
kg 1057 Mp
Solar Fusion Cycle 2e- 4p ? 4He 2n 26.7
MeV (thermal) Rn Neutrino rate 2 L/26.7MeV
1.8x1038 n/sec Flux at earth Rn/(4pR2)
6x1010/cm2/sec
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flux vs radius
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Super Kamiokande Experiment
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Neutrinos Point Back to the Sun!
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The Story of Cosmic Rays
R. A. Millikan - 1925
Victor Hess 1911 (Nobel prize 1936)
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The Cosmic Ray Energy Spectrum

• E-3
• Knee
• Ankle

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Sources
??
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GZK Cutoff

• p g p p0 (Interaction with CMB)
• Eth 1020 eV
• lint 20 Mpc

mp (MN mp/2) 2 Eg
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Shower Detection
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HiRes AGASA Comparison
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Pierre Auger Observatory(Malargue, Argentina)
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New Result from Auger (2007)
From A. Olinto
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AUGER sees correlations with nearby Active
Galactic Nuclei
Egt 6x1019eV
"Correlation of the Highest-Energy Cosmic Rays
with Nearby Extragalactic Objects, The Pierre
Auger Collaboration (9 November 2007) Science 318
(5852), 938.