High-resolution shape model of Ceres from stereophotoclinometry using Dawn Imaging Data

Park, Ryan; Vaughan, Andrew T M; Konopliv, Alexander S.; Ermakov, A.; Mastrodemos, N.; Castillo‐Rogez, Julie; Joy, S. P.; Nathues, A.; Polanskey, C.; Rayman, Marc D.; Riedel, Joseph E.; Raymond, C. A.; Russell, C. T.; Zuber, M. T.

doi:10.1016/j.icarus.2018.10.024

Cited by 58 publications

(41 citation statements)

References 27 publications

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“…The transformation between the probability density functions of the 1‐D and 2‐D slopes has been found in Kreslavsky et al (), assuming uniform (isotropic) distribution of the steepest descent azimuths:

f_{1 D} false(p false) = \frac{1}{π} \int_{0}^{π false/ 2} f_{2 D} ((), \frac{false| p false|}{\cos ϕ}) \frac{dϕ}{\cos ϕ},

f_{2 D} false(s false) = - 2 \frac{d}{ds} ([], s \int_{0}^{π false/ 2} f_{1 D} ((), \frac{s}{\cos ϕ}) \frac{dϕ}{\cos^{2} ϕ}),

where s is the 2‐D slope, p is the 1‐D slope, and ϕ is the integration variable. Park et al () checked the distribution of the North‐South and East‐West slopes of Ceres and found that they are nearly identical. We came to the same conclusion with Vesta's North‐South and East‐West 1‐D slope distributions.…”

Section: Methodsmentioning

confidence: 99%

“…Therefore, for this study we also decided to use the SPC shape model due to its higher resolution. The total height error of the Ceres SPC shape model is 10.2 m and 88.9% of the surface has the total height error below 20 m (Park et al, ).…”

Section: Datamentioning

confidence: 99%

“…The difference between the polar and equatorial axes of the best fit ellipsoids is ≈56 km for Vesta and ≈36 km for Ceres. The long‐wavelength content of the shape models has been used along with the gravity field models (Konopliv, Park, et al, , ; Park et al, , ) to constrain the internal structure of these bodies (see Ermakov, Mazarico, et al, ; Fu et al, , for Vesta and Ermakov, Mazarico, et al, ; Fu et al, , for Ceres). However, the short‐wavelength topography, at scales of 10–100 image pixels (several kilometers‐scale and shorter) from the lowest altitude orbit, has not been characterized in a statistical sense.…”

Section: Introductionmentioning

confidence: 99%

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Surface Roughness and Gravitational Slope Distributions of Vesta and Ceres

et al. 2019

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Heavily cratered terrains dominate the surfaces of asteroid 4 Vesta and dwarf planet 1 Ceres. The data from the Dawn spacecraft allowed reconstruction of high‐resolution shape models of these bodies. We used the stereophotoclinometric shape models to compute gravitational slopes and topographic roughness of Vesta and Ceres. We compute the slope distributions of Vesta and Ceres and compare them to those of the other bodies with heavily cratered terrains. The distribution of slopes of Vesta and Ceres has a kink at ≈34°. The slope distribution is steeper for slopes higher than ≈34°. The Moon and Mars have a similar kink but at a lower (shallower) slope (≈29°–30°). We hypothesize that this kink corresponds to the angle of repose, which is higher on the two minor bodies compared to that of Mars and the Moon. We have also analyzed the topographic roughness of Vesta and Ceres. Vesta's topography is characterized by lower roughness in the southern hemisphere that was resurfaced by giant impacts. The roughness of Ceres is mostly controlled by regional‐scale geology with no significant large‐scale variations. Large, fresh craters have smooth ejecta blankets on both Vesta and Ceres unlike previously observed rough ejecta on the Moon, Mars, and Mercury. On Ceres, the smooth ejecta craters also have smooth floors explained by impact slurry. Lineaments of elevated roughness are abundant on Ceres, whereas are nearly absent on Vesta. The roughness maps we produced provide a synoptic view of the surface texture and could be used to aid geologic mapping.

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f_{1 D} false(p false) = \frac{1}{π} \int_{0}^{π false/ 2} f_{2 D} ((), \frac{false| p false|}{\cos ϕ}) \frac{dϕ}{\cos ϕ},

f_{2 D} false(s false) = - 2 \frac{d}{ds} ([], s \int_{0}^{π false/ 2} f_{1 D} ((), \frac{s}{\cos ϕ}) \frac{dϕ}{\cos^{2} ϕ}),

Section: Methodsmentioning

confidence: 99%

Section: Datamentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Surface Roughness and Gravitational Slope Distributions of Vesta and Ceres

et al. 2019

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“…The locations and areas of water ice detections are given in Combe et al (). Slopes and aspects given in Table were measured from the Low Altitude Mapping Orbit (LAMO) DTM (Park et al, , https://sbn.psi.edu/pds/resource/dawn/dwncfcshape.html). Framing Camera images used to calculate water ice patch albedos in Table are the image IDs referenced by Combe et al () in the identification of the water ice patches and are archived on the Planetary Data System.…”

Section: Acknowledgmentsmentioning

confidence: 99%

“…The locations and areas of water ice detections are given in Combe et al (2018). Slopes and aspects given in Table 1 were measured from the Low Altitude Mapping Orbit (LAMO) DTM (Park et al, 2019, https://sbn.psi.edu/ pds/resource/dawn/dwncfcshape. html).…”

Section: 1029/2018je005780mentioning

confidence: 99%

Water Vapor Contribution to Ceres' Exosphere From Observed Surface Ice and Postulated Ice‐Exposing Impacts

et al. 2019

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Telescopic observations have detected an exosphere around Ceres, composed of either water vapor or its photolytic products. Proposed mechanisms for its formation include sublimation or sputtering from solar energetic particles of buried ice, surface ice, or an optically thin seasonal polar cap. We estimate the amount of water vapor produced by known exposures of water ice, detected in Dawn spacecraft image and spectral data and by ice exposures from subresolution impact craters. We use thermal and sublimation modeling to take into account slope, orientation, and, in the case of water ice within craters, shadowing due to crater walls. We use a Monte Carlo approach to calculate the number of ice‐exposing impacts, where they occur on Ceres' surface, and how long the ice within the impact crater remains bright (e.g., less than one monolayer of sublimation lag). We find that the observed water ice patches on Ceres could account for ~0.06 kg/s of water vapor to (with Oxo crater as the main contributor) and that ice‐exposing impacts that remain bright in appearance after one Ceres year supply 0.08–0.56 kg/s of vapor, depending on the regolith volume fraction of the ice. While water ice has not been detected to date at Occator crater, if it were present we find that Occator is unlikely to be a major contributor of vapor. We find a typical background water vapor production rate from all of Ceres, combining surface and buried ice, of about a few tenths of a kilogram per second.

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Replenishment of near-surface water ice by impacts into Ceres' volatile-rich crust: Observations by Dawn's Gamma Ray and Neutron Detector

Prettyman

Yamashita

Landis

et al. 2021

Preprint

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show abstract

High-resolution shape model of Ceres from stereophotoclinometry using Dawn Imaging Data

Cited by 58 publications

References 27 publications

Surface Roughness and Gravitational Slope Distributions of Vesta and Ceres

Surface Roughness and Gravitational Slope Distributions of Vesta and Ceres

Water Vapor Contribution to Ceres' Exosphere From Observed Surface Ice and Postulated Ice‐Exposing Impacts

Replenishment of near-surface water ice by impacts into Ceres' volatile-rich crust: Observations by Dawn's Gamma Ray and Neutron Detector

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