Thermophysical modeling of main-belt asteroids from WISE thermal data
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F18%3A10385761" target="_blank" >RIV/00216208:11320/18:10385761 - isvavai.cz</a>
Result on the web
<a href="https://doi.org/10.1016/j.icarus.2018.03.016" target="_blank" >https://doi.org/10.1016/j.icarus.2018.03.016</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1016/j.icarus.2018.03.016" target="_blank" >10.1016/j.icarus.2018.03.016</a>
Alternative languages
Result language
angličtina
Original language name
Thermophysical modeling of main-belt asteroids from WISE thermal data
Original language description
By means of a varied-shape thermophysical model of Harm et al. (2015) 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 less than or similar to 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).
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
Result was created during the realization of more than one project. More information in the Projects tab.
Continuities
P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)
Others
Publication year
2018
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Icarus
ISSN
0019-1035
e-ISSN
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Volume of the periodical
309
Issue of the periodical within the volume
Neuveden
Country of publishing house
US - UNITED STATES
Number of pages
41
Pages from-to
297-337
UT code for WoS article
000433400500020
EID of the result in the Scopus database
2-s2.0-85044459181