Vesta surface thermal properties map

Capria, M. T.; Tosi, F.; Sanctis, M. C. De; Capaccioni, F.; Ammannito, E.; Frigeri, Alessandro; Zambon, F.; Fonte, S.; Palomba, E.; Turrini, D.; Titus, T. N.; Schröder, Stefan; Toplis, Michael J.; Li, J.-Y.; Combe, Jean-Philippe; Raymond, C. A.; Russell, C. T.

doi:10.1002/2013gl059026

Cited by 52 publications

(67 citation statements)

References 40 publications

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“…The Cornelia pitted terrain is more than 10°colder than the surrounding terrain (Tosi et al, 2013) and has a high thermal inertia . This suggests that these materials have an increased density and/or thermal conductivity compared to the surrounding terrain, which is consistent with the model of pitted terrain formation due to devolatilization (Tosi et al, 2013;Capria et al, 2014). The pitted floor terrain in Cornelia is more extensive and distinct than that in Numisia (Denevi et al, 2012) and most likely is in-place material, not a slump deposit.…”

Section: Cornelia Cratersupporting

confidence: 79%

The unique geomorphology and physical properties of the Vestalia Terra plateau

Buczkowski¹,

Wyrick²,

Toplis³

et al. 2014

Icarus

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a b s t r a c tWe produced a geologic map of the Av-9 Numisia quadrangle of asteroid Vesta using Dawn spacecraft data to serve as a tool to understand the geologic relations of surface features in this region. These features include the plateau Vestalia Terra, a hill named Brumalia Tholus, and an unusual ''dark ribbon'' material crossing the majority of the map area. Stratigraphic relations suggest that Vestalia Terra is one of the oldest features on Vesta, despite a model crater age date similar to that of much of the surface of the asteroid. Cornelia, Numisia and Drusilla craters reveal bright and dark material in their walls, and both Cornelia and Numisia have smooth and pitted terrains on their floors suggestive of the release of volatiles during or shortly after the impacts that formed these craters. Cornelia, Fabia and Teia craters have extensive bright ejecta lobes. While diogenitic material has been identified in association with the bright Teia and Fabia ejecta, hydroxyl has been detected in the dark material within Cornelia, Numisia and Drusilla. Three large pit crater chains appear in the map area, with an orientation similar to the equatorial troughs that cut the majority of Vesta. Analysis of these features has led to several interpretations of the geological history of the region. Vestalia Terra appears to be mechanically stronger than the rest of Vesta. Brumalia Tholus may be the surface representation of a dike-fed laccolith. The dark ribbon feature is proposed to represent a long-runout ejecta flow from Drusilla crater.

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Section: Cornelia Cratersupporting

confidence: 79%

The unique geomorphology and physical properties of the Vestalia Terra plateau

Buczkowski¹,

Wyrick²,

Toplis³

et al. 2014

Icarus

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“…We performed the analysis of the thermal properties of the surface of Ceres by using the same procedure previously adopted for Vesta (Capria et al, ). We selected the data from the Survey and HAMO mission phases, as they display a good tradeoff between coverage and pixel resolution compared to other mission phases (Figure ).…”

Section: Thermophysical Analysis Of the Surface Of Ceresmentioning

confidence: 99%

High Thermal Inertia Zones on Ceres From Dawn Data

et al. 2020

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Thermal inertia is a key information to quantify the physical status of a planetary surface. We derive the thermal inertia of the surface of Ceres using spatially resolved data from the Dawn mission. For each location, this quantity can be constrained by comparing theoretical and observed diurnal temperature profiles from retrieved temperatures. We calculated Ceres's surface theoretical temperatures with a thermophysical model that provides temperature as a function of thermal conductivity and roughness, and we determined the values of those parameters for which the best fit with the observed data is obtained. Our results suggest that the area of crater Haulani displays thermal inertia values (up to 130–140 J·m−2·s−½·K−1) substantially higher than the very low to low values (from 1–15 to 50–60 J·m−2·s−½·K−1) derived for the overall surface of Ceres. The results are more ambiguous for the bright faculae located in the floor of crater Occator.

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“…For a detailed discussion of the results from mid-IR observations of small bodies carried out by in situ missions such as Dawn and Rosetta, the reader is referred to chapters by Barucci et al and Russel et al (this volume). These missions gathered thermal IR maps of bodies such as (2867) Steins (Leyrat et al 2011), (21) Lutetia, and (4) Vesta (Keihm et al 2012;Tosi et al 2014;Capria et al 2014). …”

Section: The Missionsmentioning

confidence: 99%

Space-Based Thermal Infrared Studies of Asteroids

Mainzer¹,

Usui²,

Trilling³

2015

Asteroids IV

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Large-area surveys operating at mid-infrared wavelengths have proven to be a valuable means of discovering and characterizing minor planets. Through the use of radiometric models, it is possible to derive physical properties such as diameters, albedos, and thermal inertia for large numbers of objects. Modern detector array technology has resulted in a significant improvement in spatial resolution and sensitivity compared with previous generations of spacebased infrared telescopes, giving rise to a commensurate increase in the number of objects that have been observed at these wavelengths. Space-based infrared surveys of asteroids therefore offer an effective method of rapidly gathering information about small body populations orbital and physical properties. The AKARI, WISE/NEOWISE, Spitzer, and Herschel missions have significantly increased the number of minor planets with well-determined diameters and albedos.

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Vesta surface thermal properties map

Cited by 52 publications

References 40 publications

The unique geomorphology and physical properties of the Vestalia Terra plateau

The unique geomorphology and physical properties of the Vestalia Terra plateau

High Thermal Inertia Zones on Ceres From Dawn Data

Space-Based Thermal Infrared Studies of Asteroids

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