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By means of a varied-shape thermophysical model (VS-TPM) of Hanus et al.(2015) that takes into account asteroid shape and pole uncertainties, weanalyze the thermal IR data acquired by the NASA's WISE satellite of about 300asteroids with derived convex shape models. We utilize publicly availableconvex shape models and rotation states as input for the TPM. For more than onehundred asteroids, the TPM gives us an acceptable fit to the thermal IR dataallowing us to report their size, thermal inertia, surface roughness or visiblegeometric albedo. This work more than doubles the number of asteroids withdetermined thermophysical properties. In the remaining cases, the shape modeland pole orientation uncertainties, specific rotation or thermophysicalproperties, poor thermal IR data or their coverage prevent the determination ofreliable thermophysical properties. Finally, we present the main results of thestatistical study of derived thermophysical parameters within the wholepopulation of main-belt asteroids and within few asteroid families. Our sizesare, in average, consistent with the radiometric sizes reported by Mainzer etal. (2016). The thermal inertia increases with decreasing size, but a largerange of thermal inertia values is observed within the similar size rangesbetween D~10-100 km. We derived unexpectedly low thermal inertias (<20 SI) forseveral asteroids with sizes 10<D<50 km, indicating a very fine and matureregolith on their surface. The thermal inertia values seem to be consistentwithin several collisional families. The fast rotators with P<4 h tend to haveslightly larger thermal inertia values, so probably are not covered by a fineregolith. This could be explained, for example, by the loss of the fineregolith due to the centrifugal force, or by the ineffectiveness of theregolith production (e.g., by the thermal cracking mechanism of Delbo' et al.2014).

Thermophysical modeling of main-belt asteroids from WISE thermal data