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We report the results of new XMM-Newton observations of the middle-aged($\sim$10$^5$ yr) radio pulsar PSR J1740+1000 carried out in 2017-2018. Theselong pointings ($\sim$530 ks) show that the non-thermal emission, welldescribed by a power-law spectrum with photon index $\Gamma=1.80\pm0.17$, ispulsed with a $\sim$30% pulsed fraction above 2 keV. The thermal emission canbe well fit with the sum of two blackbodies of temperatures $kT_1=70\pm4$ eV,$kT_2=137\pm7$ eV, $R_1=5.4_{-0.9}^{+1.3}$ km and $R_2=0.70_{-0.13}^{+0.15}$ km(for a distance of 1.2 kpc). We found no evidence for absorption lines as thoseobserved in the shorter XMM-Newton observations ($\sim$67 ks) of this pulsarcarried out in 2006. The X-ray thermal and non-thermal components peak inanti-phase and none of them is seen to coincide in phase with the radio pulse.This, coupled with the small difference in the emission radii of the twothermal components, disfavors an interpretation in which the dipolar polar capis heated by magnetospheric backward-accelerated particles. Comparison with theother thermally-emitting isolated neutron stars with spectra well described bythe sum of two components shows that the ratios $T_2$/$T_1$ and $R_2$/$R_1$ aresimilar for objects of different classes. The observed values cannot bereproduced with simple temperature distributions, such as those caused by adipolar field, indicating the presence of more complicated thermal maps.

Thermal and non-thermal X-ray emission from the rotation-powered radio/$\gamma$-ray pulsar PSR J1740+1000