Table 2: Comparison of observed and theoretical $\gamma $-ray luminosity for confirmed high-energy $\gamma $-ray pulsars.

PSR		 P B12 d $\alpha$ $f(\bar{r})$ $\eta^{\rm th}_{\gamma}$ $\eta^{\rm ob}_{\gamma} $
  (s) (G) (kpc) (deg.)   (%) (%)
B0531+21 0.033 7.53 2.0 $\sim$72 0.04 0.006 $0.013\pm0.006$
B0833-45 0.089 6.75 0.3 $\sim$28 0.10 0.102 $0.065\pm0.025$
B0633+17 0.237 3.28 0.16 $\sim$40 0.53 15.0 $5.0\pm4.0$
B1706-44 0.1025 6.25 1.82 $\sim$60 0.15 0.35 $0.72\pm0.47$
B1951+32 0.0395 0.97 2.5 $\sim$58 0.13 0.23 $0.26\pm0.17$
B1046-58 0.124 6.98 2.98 $\sim$68 0.20 0.82 $1.1\pm 0.3$
B1055-52 0.197 2.17 1.53 $\sim$63 0.64 25.6 $15\pm 7$
Note: the inclination angle for each pulsar is estimated by using
X-ray observed data in the frame of our model.

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