10 0 10 1 10 2 10 3 10 4 10 5 10 -2 10 -1 10 0 10 1 10 2 10 3 10 4 dN/dln   (MeV) Light cylinder 1.2R 2R 5R 20R 10 -1 10 0 10 1 10 2 10 3 10 4  (MeV) Light cylinder 1.2R 2R 5R 20R 10 -1 10 0 10 1 10 2 10 3 10 4 10 5  (MeV) Light cylinder 1.2R 2R 5R 20R 10 0 10 1 10 2 10 3 10 4 10 1 10 2 10 3 10 4 dN/dln E E (MeV) Light cylinder r=1.2R 2R 10 2 10 3 10 4 E (MeV) Light cylinder r=1.05R 1.2R 2R 5R 10 2 10 3 10 4 10 5 E (MeV) Light cylinder r=1.05R 1.2R 2R 5R 22 Zach Medin and Dong Lai 10 1 10 2 10 3 10 4 10 5 10 -2 10 -1 10 0 10 1 10 2 10 3 10 4 10 5 dN/dln   (MeV) ICS, warm spot Cool spot No ICS 10 1 10 2 10 3 10 4 10 1 10 2 10 3 10 4 10 5 dN/dln E E (MeV) ICS, warm spot Cool spot No ICS Figure 15. The effect of resonant inverse Compton scattering on the final photon and pair spectra. Two surface hot spot models are considered: a “warm” spot ( T$_{6}$ = 1, θ$_{spot}$ = 0 . 3) and “cool” spot ( T$_{6}$ = 0 . 3, θ$_{spot}$ = π/ 2). The case where ICS is inactive is also shown. The other cascade parameters are: B$_{p,}$$_{12}$ = 44 . 14, P$_{0}$ = 1 (a dipole field geometry is used), and γ$_{0}$ = 4 × 10 $^{7}$. The photon spectra are shown in the left panel and the pair spectra are shown in the right panel. Figure 14. The cumulative photon and pair spectra at magnetosphere radii r = 1 . 05 R , 1 . 2 R , 2 R , 5 R , 20 R , and r$_{LC}$ (denoted “Light cylinder”), for B$_{p,}$$_{12}$ = 1 (left two panels), 44 . 14 (middle panels), and 1000 (right panels). The NS spin period is P$_{0}$ = 1 and a dipole field geometry is used, and γ$_{0}$ = 2 × 10 $^{7}$. The photon spectra are shown in the top three panels; the pair spectra are shown in the bottom three panels. For a given magnetosphere radius r , every cascade particle that is created below r and survives until reaching r is recorded in the spectrum.