Thermophysical modeling of main-belt asteroids from WISE thermal data
| Type of publication: | Article |
| Citation: | |
| Publication status: | Published |
| Journal: | Icarus |
| Volume: | 309 |
| Year: | 2018 |
| Month: | jul |
| Pages: | 297--337 |
| ISSN: | 0019-1035 |
| URL: | https://ui.adsabs.harvard.edu/... |
| Abstract: | By means of a varied-shape thermophysical model of Hanuš et al. (2015) |
| Userfields: | ={that takes into account asteroid shape and pole uncertainties, we, analyze the thermal infrared data acquired by the NASA's Wide-field, Infrared Survey Explorer of about 300 asteroids with derived convex, shape models. We utilize publicly available convex shape models and, rotation states as input for the thermophysical modeling. For more than, one hundred asteroids, the thermophysical modeling gives us an, acceptable fit to the thermal infrared data allowing us to report their, thermophysical properties such as size, thermal inertia, surface, roughness or visible geometric albedo. This work more than doubles the, number of asteroids with determined thermophysical properties,, especially the thermal inertia. In the remaining cases, the shape model, and pole orientation uncertainties, specific rotation or thermophysical, properties, poor thermal infrared 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 based on TPM 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 J m-2 s- 1 / 2 K-1) for several, asteroids with sizes 10 < D < 50 km, indicating a very fine and, mature regolith on these small bodies. The thermal inertia values seem, to be consistent within several collisional families, however, the, statistical sample is in all cases rather small. The fast rotators with, rotation period P ≲ 4 h tend to have slightly larger thermal inertia, values, so probably do not have a fine regolith on the surface. 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). , 10.1016/j.icarus.2018.03.016, eprint: arXiv:1803.06116}, |
| Keywords: | Asteroids, Astrophysics - Earth and Planetary Astrophysics, composition, Infrared observations, Photometry, surfaces |
| Authors | |
| Added by: | [JoH] |
| Total mark: | 0 |
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