Table 1: Pulsed X-ray properties of rotation-powered pulsars. Comparison of model X-ray luminosity ( $L^{\rm th}_{\rm X}$) (assuming $\alpha =55^{\circ }$) with observed pulsed X-ray luminosity ( $L^{\rm ob}_{\rm X}$) for each X-ray pulsars.

PSR		 P B12 d $\log(L^{\rm th}_{\rm X})$ $\log(L^{\rm ob}_{\rm X})$
  s G kpc erg/s erg/s
J0631+1036 0.288 10.86 1.0 30.78 31.30
J1811-1926 0.065 3.42 5.0 32.81 33.28
B0531+21 0.033 7.53 2.0 34.98 35.83
B0833-45 0.089 6.75 0.3 32.79 32.18
B0633+17 0.237 3.28 0.16 30.06 29.66
B1706-44 0.1025 6.25 1.82 32.42 32.61
B1509-58 0.150 30.76 4.3 33.12 34.11
B1951+32 0.0395 0.97 2.5 32.68 32.79
B1046-58 0.124 6.98 2.98 32.13 32.74
B1929+10 0.227 1.04 0.17 29.07 29.74
B0656+14 0.385 9.31 0.76 30.02 31.00
B0540-69 0.05 9.91 49.4 34.36 36.11
B0950+08 0.253 0.49 0.12 28.14 29.20
B1610-50 0.232 21.64 7.26 31.88 33.48
B1055-52 0.197 2.17 1.53 30.06 30.30
B1853+01 0.267 20.43 2.02 31.53 32.15
J2229+6114 0.0516 4.06 3.0 33.46 32.60
B0537-69 0.016 1.83 47.0 35.17 35.23
J1846-0258 0.32 96.47 19.0 32.61 34.60
Note: the pulsed X-ray luminosity of pulsars have $30\%$uncertainty except for B1706-44, B1046-58, and J1610-50 which have a $50\%$ uncertainty (Cheng et al. 2004). The magnetic field strength is given by $B_{12}\approx 6.4\times 10^{7}(P\dot{P})^{1/2}$.

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