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

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FIG. 5: The energy spectra of γ-rays contributed by secondaries produced in CR (p and α)+ISM interactions, assuming an exponential cutoff in the cosmic-ray spectrum at 100 TeV described in Eq. (10). The plots are arranged as in Figure 4. 24
FIG. 6: Diffuse γ-ray spectrum at GeV range, shown in comparison with data for the inner part of Galaxy at 315 0 ≤ l ≤ 345 0 and |b| ≤ 5 0 [6]. The model spectrum is composed of a hadronic component calculated with cosmic-ray spectrum according to Eq. (10), plus a power-law component with spectral index Γ e = 2.1 for bremsstrahlung. Different curves correspond to different normalizations of the hadronic and leptonic contributions, here by varying the electron energy density ω e = 0.1, 0.4, 0.8 eV/cm 3 and the gas column density N ISM = 3 × 10 22 , 8 × 10 21 , 3 × 10 21 cm −2 . The energy density of hadronic cosmic rays is kept constant at ρ E = 0.75 eV/cm 3 . 25
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 and 22: FIG. 2: The energy spectra of the
Page 23: FIG. 4: The energy spectra of γ-ra
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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