Geologic mapping of Vesta

Yingst, R. A.; Mest, S. C.; Berman, D. C.; Garry, W. B.; Williams, D. A.; Buczkowski, D. L.; Jaumann, R.; Pieters, C. M.; Sanctis, M. C. De; Frigeri, Alessandro; Corre, Lucille Le; Preusker, Frank; Raymond, C. A.; Reddy, V.; Russell, C.T.; Roatsch, Thomas; Schenk, P.

doi:10.1016/j.pss.2013.12.014

Cited by 64 publications

(99 citation statements)

References 55 publications

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“…The mapping was based on the Digital Cartographic Standard for Geologic Map Symbolization defined by the U.S. Geological Survey (2006) and Nass et al (2011) and performed using ESRI's software package ArcGIS. The RGB (red, green, blue) color code for the geologic units was defined after the one used in the Vesta global map by Yingst et al (2014).…”

Section: Datasets and Methodsmentioning

confidence: 99%

“…The unit exhibits lobate tongues or fan-shapes and a smooth to hummocky surface on the crater walls (Jaumann et al, 2012;Yingst et al, 2014). The unit also appears as spur-and-gully morphologies on the crater and scarp walls.…”

Section: Geologic Settingmentioning

confidence: 99%

“…Interpretation: These features are interpreted as debris fall, slump or slide through slope failure associated with a number of possible processes, including ''seismic'' shaking associated with impact crater formation or slope failure due to overburden (Williams et al, 2013;Yingst et al, 2014).…”

Section: Geologic Settingmentioning

confidence: 99%

“…To understand the geologic history of Vesta, a global geologic map, at a scale of 1:500,000 (Yingst et al, 2014) and a set of 15 quadrangle maps (Fig. 1) at a scale of 1:250,000 in more detail were produced by the Dawn Science Team (Roatsch et al, 2012(Roatsch et al, , 2013Williams et al, this issue).…”

Section: Introductionmentioning

confidence: 99%

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Mass movement on Vesta at steep scarps and crater rims

Krohn

Jaumann

Otto

et al. 2014

Icarus

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a b s t r a c tThe Quadrangles Av-11 and Av-12 on Vesta are located at the northern rim of the giant Rheasilvia south polar impact basin. The primary geologic units in Av-11 and Av-12 include material from the Rheasilvia impact basin formation, smooth material and different types of impact crater structures (such as bimodal craters, dark and bright crater ray material and dark ejecta material). Av-11 and Av-12 exhibit almost the full range of mass wasting features observed on Vesta, such as slump blocks, spur-and-gully morphologies and landslides within craters. Processes of collapse, slope instability and seismically triggered events force material to slump down crater walls or scarps and produce landslides or rotational slump blocks. The spur-and-gully morphology that is known to form on Mars is also observed on Vesta; however, on Vesta this morphology formed under dry conditions.

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Section: Datasets and Methodsmentioning

confidence: 99%

Section: Geologic Settingmentioning

confidence: 99%

Section: Geologic Settingmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Mass movement on Vesta at steep scarps and crater rims

Krohn

Jaumann

Otto

et al. 2014

Icarus

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“…In contrast, according to Yingst et al (2014) Lucaria Tholus is a remnant of a volcanic feature (dike, intrusion, or volcanic cone), which has been exposed by impacts.…”

Section: Pre-veneneian Period: Tholus Materials (T)mentioning

confidence: 99%

Imprint of the Rheasilvia impact on Vesta – Geologic mapping of quadrangles Gegania and Lucaria

Schäfer¹,

Nathues²,

Williams³

et al. 2014

Icarus

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a b s t r a c tWe produced two 1:250,000 scale geologic maps of the adjacent quadrangles Av-6 Gegania and Av-7 Lucaria, located in the equatorial region of (4) Vesta (0-144°E, 22°S to 22°N). The mapping is based on clear and color filter images of the Framing Camera (FC) onboard the Dawn spacecraft, which has captured the entire illuminated surface of Vesta with high spatial resolution (up to $20 m/pixel), and on a digital terrain model derived from FC imagery. Besides the geologic mapping itself, a secondary purpose of this work is to investigate one of the most prominent morphological features on Vesta, namely the aggregation of several giant equatorial troughs termed the Divalia Fossae, most probably formed during the Rheasilvia impact near Vesta's south pole. The up to 465 km long and 22 km wide troughs show height differences of up to 5 km between adjacent troughs and ridges. Another imprint of the Rheasilvia impact is the >350 km long and $250 km wide swath of ejecta crossing quadrangle Av-6 Gegania. This lobe shows a distinct appearance in FC color ratios and a high albedo in FC images, indicating a mineralogical similarity to material typically found within the Rheasilvia basin, in particular composed of diogenite-rich howardites. Almost the entire northern half of the mapping area shows the oldest surface, being dominated by upper crustal basaltic material. To the south, increasingly younger formations related to the Rheasilvia impact occur, either indicated by the troughs formed by Rheasilvia or by the Rheasilvia ejecta itself. Only medium sized impact craters with diameters less than 22 km occur within the two mapped quadrangles. Some of the craters exhibit ejecta blankets and/or distinctly dark or bright ejecta material in ejecta rays outside and exposures within the crater, and mass-wasting deposits down crater slopes, forming the youngest surfaces.

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Compositional evidence of magmatic activity on Vesta

Sanctis

Ammannito

Buczkowski

et al. 2014

Geophys. Res. Lett.

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Like the Earth and other terrestrial planets, the asteroid Vesta has a basaltic crust and a large iron core; its surface is dominated by impact craters of all sizes and has tectonic features. The presence of basaltic compositions, olivine, howardite-eucrite-diogenite meteorites, and models of Vesta's formation, suggests that volcanic and/or magmatic activity could have occurred on Vesta. A global search for lobate structures did not find unequivocal evidence of volcanic features. Nevertheless, several morphological properties of Brumalia Tholus on Vestalia Terra suggest that this topographic high most likely formed as a magmatic intrusion. The presence of more orthopyroxene-rich material relative to surrounding terrain in the ejecta of Teia, a fresh impact crater on the northern face of Brumalia Tholus, supports the hypothesis of magmatic intrusions on Vesta.

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Geologic mapping of Vesta

Cited by 64 publications

References 55 publications

Mass movement on Vesta at steep scarps and crater rims

Mass movement on Vesta at steep scarps and crater rims

Imprint of the Rheasilvia impact on Vesta – Geologic mapping of quadrangles Gegania and Lucaria

Compositional evidence of magmatic activity on Vesta

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