TY  - JOUR
T1  - Thermophysical modeling of main-belt asteroids from WISE thermal data
A1  - Hanuš, J.
A1  - Delbo', M.
A1  - Ďurech, J.
A1  - Alí-Lagoa, V.
JA  - Icarus
Y1  - 2018
VL  - 309
SP  - 297
EP  - 337
SN  - 0019-1035
UR  - https://ui.adsabs.harvard.edu/abs/2018Icar..309..297H
KW  - Asteroids
KW  - Astrophysics - Earth and Planetary Astrophysics
KW  - composition
KW  - Infrared observations
KW  - Photometry
KW  - surfaces
N2  - By means of a varied-shape thermophysical model of Hanuš et al. (2015)
M1  - ={that takes into account asteroid shape and pole uncertainties
M1  -  we
M1  -  analyze the thermal infrared data acquired by the NASA's Wide-field
M1  -  Infrared Survey Explorer of about 300 asteroids with derived convex
M1  -  shape models. We utilize publicly available convex shape models and
M1  -  rotation states as input for the thermophysical modeling. For more than
M1  -  one hundred asteroids
M1  -  the thermophysical modeling gives us an
M1  -  acceptable fit to the thermal infrared data allowing us to report their
M1  -  thermophysical properties such as size
M1  -  thermal inertia
M1  -  surface
M1  -  roughness or visible geometric albedo. This work more than doubles the
M1  -  number of asteroids with determined thermophysical properties
M1  -  especially the thermal inertia. In the remaining cases
M1  -  the shape model
M1  -  and pole orientation uncertainties
M1  -  specific rotation or thermophysical
M1  -  properties
M1  -  poor thermal infrared data or their coverage prevent the
M1  -  determination of reliable thermophysical properties. Finally
M1  -  we present
M1  -  the main results of the statistical study of derived thermophysical
M1  -  parameters within the whole population of main-belt asteroids and within
M1  -  few asteroid families. Our sizes based on TPM are
M1  -  in average
M1  -  consistent with the radiometric sizes reported by Mainzer et al. (2016).
M1  -  The thermal inertia increases with decreasing size
M1  -  but a large range of
M1  -  thermal inertia values is observed within the similar size ranges
M1  -  between D ∼ 10-100 km. We derived unexpectedly low thermal inertias (
M1  -  &lt; 20 J m-<SUP>2</SUP> s<SUP>- 1 / 2</SUP> K-<SUP>1</SUP>) for several
M1  -  asteroids with sizes 10 &lt; D &lt; 50 km
M1  -  indicating a very fine and
M1  -  mature regolith on these small bodies. The thermal inertia values seem
M1  -  to be consistent within several collisional families
M1  -  however
M1  -  the
M1  -  statistical sample is in all cases rather small. The fast rotators with
M1  -  rotation period P ≲ 4 h tend to have slightly larger thermal inertia
M1  -  values
M1  -  so probably do not have a fine regolith on the surface. This
M1  -  could be explained
M1  -  for example
M1  -  by the loss of the fine regolith due to
M1  -  the centrifugal force
M1  -  or by the ineffectiveness of the regolith
M1  -  production(e.g.
M1  -  by the thermal cracking mechanism of Delbo' et al.
M1  -  2014). <P />
M1  -  10.1016/j.icarus.2018.03.016
M1  -  eprint: arXiv:1803.06116}
ER  -