\begin{table}%T1
\caption{\label{tab1}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. }
 \small%\centerline
{
\begin{tabular}{llllll}
\hline\hline \noalign{\smallskip}
PSR & $P$ & $B_{12}$ & $d$  &  $\log(L^{\rm th}_{\rm X})$ & $\log(L^{\rm ob}_{\rm X})$
\\
& s & G & kpc & erg/s & erg/s \\
\hline
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 \\
\hline
\end{tabular}}
\smallskip
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 $B_{12}\approx 6.4\times 10^{7}(P\dot{P})^{1/2}$.
\end{table}