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

• Published in: Icarus
• Other Authors: Ruesch, Ottaviano (Author), Hiesinger, Harald (Author), Blewett, David T. (Author), Williams, David (ASU author), Buczkowski, Debra (Author), Scully, Jennifer (Author), Yingst, R. Aileen (Author), Roatsch, Thomas (Author), Preusker, Frank (Author), Jaumann, Ralf (Author), Russell, Christopher T. (Author), Raymond, Carol A. (Author), College of Liberal Arts and Sciences, School of Earth and Space Exploration
• Format: Text
• Language: English
• Published: 2014
• Subjects: South Pole; South pole
• Online Access: https://doi.org/10.1016/j.icarus.2014.01.035; http://hdl.handle.net/2286/R.I.28055

abstract: The Dawn Framing Camera (FC) has imaged the northern hemisphere of the Asteroid (4) Vesta at high spatial resolution and coverage. This study represents the first investigation of the overall geology of the northern hemisphere (22–90°N, quadrangles Av-1, 2, 3, 4 and 5) using these unique Dawn mission observations. We have compiled a morphologic map and performed crater size–frequency distribution (CSFD) measurements to date the geologic units. The hemisphere is characterized by a heavily cratered surface with a few highly subdued basins up to ∼200 km in diameter. The most widespread unit is a plateau (cratered highland unit), similar to, although of lower elevation than the equatorial Vestalia Terra plateau. Large-scale troughs and ridges have regionally affected the surface. Between ∼180°E and ∼270°E, these tectonic features are well developed and related to the south pole Veneneia impact (Saturnalia Fossae trough unit), elsewhere on the hemisphere they are rare and subdued (Saturnalia Fossae cratered unit). In these pre-Rheasilvia units we observed an unexpectedly high frequency of impact craters up to ∼10 km in diameter, whose formation could in part be related to the Rheasilvia basin-forming event. The Rheasilvia impact has potentially affected the northern hemisphere also with S–N small-scale lineations, but without covering it with an ejecta blanket. Post-Rheasilvia impact craters are small (<60 km in diameter) and show a wide range of degradation states due to impact gardening and mass wasting processes. Where fresh, they display an ejecta blanket, bright rays and slope movements on walls. In places, crater rims have dark material ejecta and some crater floors are covered by ponded material interpreted as impact melt. NOTICE: this is the author's version of a work that was accepted for publication in ICARUS. Changes may have been made to this work since it was submitted for publication. A definitive version was subsequently published in ICARUS, 244, 41-59. DOI:10.1016/j.icarus.2014.01.035