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

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FIG. 3: The energy loss rate for p + ISM collisions as calculated by integrating the secondary particle yield. The thick dash-dot line shows an analytical approximation. 22
FIG. 4: The energy spectra of γ-rays contributed by the secondaries produced in CR (p and α) + ISM interactions with a simple power-law cosmic-ray spectral distribution in (9). Figures are shown for baryonic (left) and mesonic (right) contributions. The total γ-ray spectrum, the components from π 0 decays and the direct γ production are also shown in each figure. Note that we only sample cosmic rays up to 10 8 GeV. 23
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 and 20: [26] T. K. Gaisser, Cosmic Rays and
Page 21: FIG. 2: The energy spectra of the
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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