Introduction to neutron astronomy

Details Introduction to neutron astronomy Introduction to neutron astronomy

Jun 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aipc..276..442c&link_type=abstract

The seventh international symposium on very high energy cosmic-ray interactions. AIP Conference Proceedings, Volume 276, pp. 44

Computer Science

1

Cosmic Rays

Scientific paper

The different channels of production of energetic neutrons in leading clusters of UHE proton collisions (for instance via Δ resonance) suggest an important neutron emission after hadronic cascading in supernovae ejection columns: typical energetic lines (versus energetic spectrum of proton accelerated from pulsars, source distance, column thickness) can be put in evidence by observing large EAS.
The situation is compared with Akeno results for a possible emission from Cygnus X3 (˜1018 eV, 11 Kpc): it appears that neutrons could be expected above 5. 106 GeV from Vela (0.5 Kpc), 2. 107 GeV from Crab (2 Kpc), 7. 107 GeV from Hercules... There are critical energies (about 2-3 times those thresholds) above which the neutron luminosity from point sources exceeds the γ-ray luminosity.

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