Geologic map of the northern hemisphere of Vesta based on Dawn Framing Camera (FC) images

Ruesch, O.; Hiesinger, H.; Blewett, D. T.; Williams, D. A.; Buczkowski, D. L.; Scully, J. E. C.; Yingst, R. A.; Roatsch, Thomas; Preusker, Frank; Jaumann, R.; Russell, C. T.; Raymond, C. A.

doi:10.1016/j.icarus.2014.01.035

Cited by 30 publications

(37 citation statements)

References 88 publications

(151 reference statements)

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“…Calpurnia just to the NE is 54 km long (N-S) by 52 km wide (E-W), and Minucia to the NE is 26 km long (N-S) by 23 km wide (E-W). The ejecta surrounding these craters dominate from the center to the northeast border of this quadrangle, and extend into the neighboring Av-4 Domitia quadrangle to the north (Roatsch et al, 2012;Ruesch et al, 2014;Scully et al, 2014).…”

Section: Dark Diffuse Unit (Spotted Pattern Overlying Other Units)mentioning

confidence: 95%

The geology of the Marcia quadrangle of asteroid Vesta: Assessing the effects of large, young craters

Williams¹,

Denevi²,

Mittlefehldt³

et al. 2014

Icarus

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a b s t r a c tWe used Dawn spacecraft data to identify and delineate geological units and landforms in the Marcia quadrangle of Vesta as a means to assess the role of the large, relatively young impact craters Marcia ($63 km diam.) and Calpurnia ($53 km diam.) and their surrounding ejecta field on the local geology. We also investigated a local topographic high with a dark-rayed crater named Aricia Tholus, and the impact crater Octavia that is surrounded by a distinctive diffuse mantle. Crater counts and stratigraphic relations suggest that Marcia is the youngest large crater on Vesta, in which a putative impact melt on the crater floor ranges in age between $40 and 60 Ma (depending upon choice of chronology system), and Marcia's ejecta blanket ranges in age between $120 and 390 Ma (depending upon choice of chronology system). We interpret the geologic units in and around Marcia crater to mark a major vestan time-stratigraphic event, and that the Marcia Formation is one of the geologically youngest formations on Vesta. Marcia crater reveals pristine bright and dark material in its walls and smooth and pitted terrains on its floor. The smooth unit we interpret as evidence of flow of impact melts and (for the pitted terrain) release of volatiles during or after the impact process. The distinctive dark ejecta surrounding craters Marcia and Calpurnia is enriched in OH-or H-bearing phases and has a variable morphology, suggestive of a complex mixture of impact ejecta and impact melts including dark materials possibly derived from carbonaceous chondrite-rich material. Aricia Tholus, which was originally interpreted as a putative vestan volcanic edifice based on lower resolution observations, appears to be a fragment of an ancient impact basin rim topped by a dark-rayed impact crater. Octavia crater has a cratering model formation age of $280-990 Ma based on counts of its ejecta field (depending upon choice of chronology system), and its ejecta field is the second oldest unit in this quadrangle. The relatively young craters and their http://dx

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Section: Dark Diffuse Unit (Spotted Pattern Overlying Other Units)mentioning

confidence: 95%

The geology of the Marcia quadrangle of asteroid Vesta: Assessing the effects of large, young craters

Williams¹,

Denevi²,

Mittlefehldt³

et al. 2014

Icarus

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“…The northern portions of both quadrangles are mapped as the unit ch, a heavily cratered terrain that shows subjectively the highest crater counts in the mapping area and thus is likely the oldest surface relatively to the other units. Unit ch is continued to the north in quadrangles Av-2 Bellicia and Av-3 Caparronia Ruesch et al, 2014). To the south, ch borders unit Df at approximately 0-5°N, and continues to the east into quadrangle Av-8 Marcia (see Williams et al, in press-b) and to the west into quadrangle Av-10 Oppia (see Garry et al, this issue).…”

Section: Geologic Settingmentioning

confidence: 98%

“…Discussion: Unit Sfc has mainly been mapped for alignment with the quadrangle Av-2 Bellicia in the north, mapped by Ruesch et al (2014), who give a detailed description. According to Ruesch et al (2014), Sfc can be interpreted as ancient vestan crustal material, which has been tectonically deformed by several large unknown impacts, unlike the Saturnalia Fossae troughs of unit Sft, which can be related to the Veneneia impact event.…”

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

confidence: 99%

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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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“…To the east are Gegania quadrangle Av-6 and Lucaria quadrangle Av-7, where troughs in the Divalia Fossae Formation are best preserved (Schäfer et al, 2014). To the north is Floronia quadrangle Av-5 (Ruesch et al, 2014;Scully et al, 2014) dominated by cratered highlands and Saturnalia Fossae Formation. To the south is Urbinia quadrangle Av-14, which is dominated by the Rheasilvia impact structure (Rheasilvia quadrangle Av-15) (see Fig.…”

Section: Geologic Setting and Features Of Oppia Quadrangle Av-10mentioning

confidence: 99%

Geologic mapping of ejecta deposits in Oppia Quadrangle, Asteroid (4) Vesta

Garry¹,

Williams²,

Yingst³

et al. 2014

Icarus

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Geologic map of the northern hemisphere of Vesta based on Dawn Framing Camera (FC) images

Cited by 30 publications

References 88 publications

The geology of the Marcia quadrangle of asteroid Vesta: Assessing the effects of large, young craters

The geology of the Marcia quadrangle of asteroid Vesta: Assessing the effects of large, young craters

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

Geologic mapping of ejecta deposits in Oppia Quadrangle, Asteroid (4) Vesta

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