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Previous works have suggested a correlation between the X-ray luminosity Lxand the rotational luminosity Lrot of the radio pulsars.However, none of theobtained regression lines are statistically acceptable due to large scatters.  We construct a statistical model which has an intrinsic Lx-Lrot relation andreproduces the observed Lx distribution about it by using a Monte Carlosimulator, which takes into account the effects obscuring the intrinsicrelation,i.e., the anisotropy of radiation, additional heating, uncertainty indistance and detection limit of the instruments.  From the ATNF pulsar catalog we collect 57 `ordinary radio pulsars' withsignificant detection and 42 with upper limits.The sample does not include thehigh-magnetic field pulsars (>10^{13} G), which are separately analyzed.  We obtain a statistically acceptable relation Lx (0.5 - 10 keV)= 10^{31.69}(Lrot / L_0)^{c_1} with c_1 = 1.03 \pm 0.27 and L_0 =10^{35.38}. Thedistribution about the obtained Lx-Lrot relation is reproduced well by thesimulator.  Pulsars with abnormally high Lx fall into two types: one is the softgamma-ray pulsars, and the other is thermally bright pulsars in comparison withthe standard cooling curve. On the other hand, pulsars showing low Lx are foundto have dim pulsar wind nebulae. We argue that there is an unknown mechanismthat governs both the magnetospheric emission and the pulsar wind nebulae, andit might involve the production rate of electron-positron pairs.  The high-field pulsars form a distinctive population other than the ordinarypulsars due to their excess luminosities.

X-ray and Rotational Luminosity Correlation and Magnetic Heating of the Radio Pulsars