  By means of a varied-shape thermophysical model (VS-TPM) of Hanus et al.
(2015) that takes into account asteroid shape and pole uncertainties, we
analyze the thermal IR data acquired by the NASA's WISE satellite of about 300
asteroids with derived convex shape models. We utilize publicly available
convex shape models and rotation states as input for the TPM. For more than one
hundred asteroids, the TPM gives us an acceptable fit to the thermal IR data
allowing us to report their size, thermal inertia, surface roughness or visible
geometric albedo. This work more than doubles the number of asteroids with
determined thermophysical properties. In the remaining cases, the shape model
and pole orientation uncertainties, specific rotation or thermophysical
properties, poor thermal IR data or their coverage prevent the determination of
reliable thermophysical properties. Finally, we present the main results of the
statistical study of derived thermophysical parameters within the whole
population of main-belt asteroids and within few asteroid families. Our sizes
are, in average, consistent with the radiometric sizes reported by Mainzer et
al. (2016). The thermal inertia increases with decreasing size, but a large
range of thermal inertia values is observed within the similar size ranges
between D~10-100 km. We derived unexpectedly low thermal inertias (<20 SI) for
several asteroids with sizes 10<D<50 km, indicating a very fine and mature
regolith on their surface. The thermal inertia values seem to be consistent
within several collisional families. The fast rotators with P<4 h tend to have
slightly larger thermal inertia values, so probably are not covered by a fine
regolith. This could be explained, for example, by the loss of the fine
regolith due to the centrifugal force, or by the ineffectiveness of the
regolith production (e.g., by the thermal cracking mechanism of Delbo' et al.
2014).
