Gamma-Rays Produced in Cosmic-Ray Interactions and TeV-band ...

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FIG. 1: π 0 and π ± production cross sections in pp collisions simulated by DPMJET-III, here shown as function of the kinetic energy E k of incident protons. The data shown figure are quoted from [10, 29, 41] 20
FIG. 2: The energy spectra of the γ-ray contributions from each secondary particle produced in p + ISM interactions for two different incident proton energies: 150 GeV (upper panel) and 10 TeV (lower panel). For ease of comparison, baryonic (left) and mesonic (right) decay contributions are separated. In each figure, the energy spectrum of total γ-rays (the sum of all contributions) and also the spectrum of the directly produced γ-ray photons are shown. 21
Page 1 and 2: Gamma-Rays Produced in Cosmic-Ray I
Page 3 and 4: I. INTRODUCTION It is generally bel
Page 5 and 6: threshold up to a few GeV [8]. In a
Page 7 and 8: the nuclear cascades in the nuclear
Page 9 and 10: For the two-body decay process, it
Page 11 and 12: generated by a cosmic-ray particle
Page 13 and 14: of cosmic-ray electrons must be exp
Page 15 and 16: in the power-law index s statistica
Page 17 and 18: collisions of cosmic rays with arbi
Page 19: [26] T. K. Gaisser, Cosmic Rays and
Page 23 and 24: FIG. 4: The energy spectra of γ-ra
Page 25 and 26: FIG. 6: Diffuse γ-ray spectrum at
Page 27 and 28: FIG. 8: The confidence regions for
Page 29 and 30: FIG. 10: The confidence regions for

Gamma-Rays Produced in Cosmic-Ray Interactions and TeV-band ...

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