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Thermal inertia of main belt asteroids smaller than 100 km from IRAS data | | Marco Delbo
; Paolo Tanga
; | | Date: |
6 Aug 2008 | | Abstract: | Recent works have shown that the thermal inertia of km-sized near-Earth
asteroids (NEAs) is more than two orders of magnitude higher than that of main
belt asteroids (MBAs) with sizes (diameters) between 200 and 1,000 km. This
confirms the idea that large MBAs, over hundreds millions of years,have
developed a fine and thick thermally insulating regolith layer, responsible for
the low values of their thermal inertia, whereas km-sized asteroids, having
collisional lifetimes of only some millions years, have less regolith, and
consequently a larger surface thermal inertia. Because it is believed that
regolith on asteroids forms as a result of impact processes, a better knowledge
of asteroid thermal inertia values and its correlation with size, taxonomic
type, and density can be used as an important constraintfor modeling of impact
processes on asteroids. However, our knowledge of asteroids’ thermal inertia
values is still based on few data points with NEAs covering the size range
0.1-20 km and MBAs that >100 km. Here, we use IRAS infrared measurements to
estimate the thermal inertias of MBAs with diameters 100 km and known shapes
and spin vector: filling an important size gap between the largest MBAs and the
km-sized NEAs. An update to the inverse correlation between thermal inertia and
diameter is presented. For some asteroids thermophysical modelling allowed us
to discriminate between the two still possible spin vector solutions derived
from optical lightcurve inversion. This is important for (720) Bohlinia: our
preferred solution was predicted to be the correct one by Vokrouhlicky et al.
(2003, Nature 425, 147) just on theoretical grounds. | | Source: | arXiv, 0808.0869 | | Services: | Forum | Review | PDF | Favorites | |
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