The Dawn Mission to Vesta and Ceres

Russell, C. T.; Raymond, C. A.

doi:10.1007/978-1-4614-4903-4_2

Cited by 72 publications

(79 citation statements)

References 22 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…The integrated approach for example science themes discussed above is summarized in Table 2. The integration of these diverse data will take some time since each of the mission phases brings increasingly more complete information from each instrument (Russell and Raymond 2011). Some of the science issues outlined above will be resolved quickly, others more slowly, and a plethora of new questions (currently unknown) will be urgently posed.…”

Section: Discussionmentioning

confidence: 99%

“…The measured depth of the GRSC is ∼13 km , suggesting that the combined suite of instruments on Dawn will look beneath the regolith deeper into the layers of the crust and/or mantle, including the cumulate eucrites studied by Miyamoto and Takeda. The Dawn mission is well suited to map the GRSC in detail and use it as a probe to the interior of Vesta. The geometry of the orbital phase of the mission favors observing the southern hemisphere of Vesta (Russell and Raymond 2011). High spatial resolution is obtained by the framing camera (FC) providing detailed geologic context, high spectral resolution across the visible and infrared is obtained by VIR providing spectroscopy needed to discriminate pyroxene composition and detect the presence of olivine or other mineral constituents, and coarse-scale (inner-vs outer-basin) elemental abundances are measured by GRaND providing a direct link to solar system materials.…”

Section: Grsc: Backgroundmentioning

confidence: 99%

See 1 more Smart Citation

Surface Composition of Vesta: Issues and Integrated Approach

et al. 2011

View full text Add to dashboard Cite

The instruments on the Dawn spacecraft are exceptionally well suited to characterize and map the surface composition of Vesta in an integrated manner. These include a framing camera with multispectral capabilities, a high spectral resolution near-infrared imaging spectrometer, and a gamma-ray and neutron spectrometer. Three examples of issues addressed at Vesta are: (1) What is the composition of Vesta's interior and differentiation state as exposed by the Great South Crater? (2) How has space weathering affected Vesta, both globally and at a local scale? and (3) Are volatiles or hydrated material present on Vesta's surface? We predict that Dawn finds many surprises, such as an olivine-bearing mantle exposed near the south-pole, a weakly or un-weathered surface that has been rela- tively recently resurfaced, and a very thin layer of surficial volatiles derived from interaction with the solar wind.

show abstract

Section: Discussionmentioning

confidence: 99%

Section: Grsc: Backgroundmentioning

confidence: 99%

Surface Composition of Vesta: Issues and Integrated Approach

et al. 2011

View full text Add to dashboard Cite

show abstract

“…The Dawn mission orbited Vesta from July 16, 2011 until September 5, 2012, using three instruments to observe the surface (Russell and Raymond, 2011). The Visual and Infrared Spectrometer (VIR) detects surface mineralogical compositions by measuring spectral variations in the range from $0.4 to 5.0 lm and corresponding absorption features (De Sanctis et al, 2010).…”

Section: Data Base and Methodsmentioning

confidence: 99%

The geological nature of dark material on Vesta and implications for the subsurface structure

Jaumann

Naß

Otto

et al. 2014

Icarus

View full text Add to dashboard Cite

a b s t r a c tDeposits of dark material appear on Vesta's surface as features of relatively low-albedo in the visible wavelength range of Dawn's camera and spectrometer. Mixed with the regolith and partially excavated by younger impacts, the material is exposed as individual layered outcrops in crater walls or ejecta patches, having been uncovered and broken up by the impact. Dark fans on crater walls and dark deposits on crater floors are the result of gravity-driven mass wasting triggered by steep slopes and impact seismicity. The fact that dark material is mixed with impact ejecta indicates that it has been processed together with the ejected material. Some small craters display continuous dark ejecta similar to lunar dark-halo impact craters, indicating that the impact excavated the material from beneath a higher-albedo surface. The asymmetric distribution of dark material in impact craters and ejecta suggests non-continuous distribution in the local subsurface. Some positive-relief dark edifices appear to be impact-sculpted hills with dark material distributed over the hill slopes. Dark features inside and outside of craters are in some places arranged as linear outcrops along scarps or as dark streaks perpendicular to the local topography. The spectral characteristics of the dark material resemble that of Vesta's regolith. Dark material is distributed unevenly across Vesta's surface with clusters of all types of dark material exposures. On a local scale, some craters expose or are associated with dark material, while others in the immediate vicinity do not show evidence for dark material. While the variety of surface exposures of dark material and their different geological correlations with surface features, as well as their uneven distribution, indicate a globally inhomogeneous distribution in the subsurface, the dark material seems to be correlated with the rim and ejecta of the older Veneneia south polar basin structure. The origin of the dark material is still being debated, however, the geological analysis suggests that it is exogenic, from carbon-rich low-velocity impactors, rather than endogenic, from freshly exposed mafic material or melt, exposed or created by impacts.

show abstract

“…The Framing Cameras (FCs) FC1 and FC2 are payloads of the Dawn spacecraft (Russell and Raymond 2012). To date (August 2017) camera FC2 has obtained ~57,000 images of Ceres in seven spectral bands (0.44 -0.98 µm) and one panchromatic filter (Sierks et al 2012), performing global color mapping of the surface of Ceres at a resolution of ~140 m/pixel (Russell et al 2016; Fig.…”

Section: Introductionmentioning

confidence: 99%