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Geology of Vulcan Planum, Charon Ross A. Beyer1,2, John R Lunar and Planetary Science XLVIII (2017) 2679.pdf Geology of Vulcan Planum, Charon Ross A. Beyer1;2, John R. Spencer3, William B. McKinnon4, Jeffrey Moore2, Stuart Robbins3, Paul Schenk5, Kelsi Singer3, Hal Weaver6, Leslie Young3, Kimberly Ennico2, Cathy Olkin3, Alan Stern3, and the New Horizons Science Team. 1Carl Sagan Center at the SETI Institute, 2NASA Ames Research Center, Moffett Field, CA, USA ([email protected]), 3SwRI, 4WUStL, 5LPI, 6JHU APL Charon has two large geologic provinces on the Kubrick Mons is also a single massif which measures Pluto-facing hemisphere that New Horizons observed 30 by 20 km in plan form and rises 3 km above the Vul- at high resolution [1]. The heavily tectonized areas of can Planum surface with a 1-km deep encircling moat. the northern regions are known as Oz Terra (this place- The surface of Kubrick is distinct from the rounded lo- name and others in this abstract are informal) and Vulcan bate shapes of Vulcan Planum which surround it. It dis- Planum is the large plain to the south. The border be- plays a ridge crest and other sharp-looking ridges that run tween them strikes diagonally across the encounter hemi- down its flanks, with a similar appearance to slopes seen sphere from as far south as −19◦ latitude in the west to on Serenity Chasma to the north. ◦ 25 in the east (Figure1). Both Vulcan Planum and Oz The Clarke Montes is a trio of peaks that sit to- Terra have a similarly old age of ∼4 Ga [2,3]. gether in a single, variable margin depression. They Vulcan Planum is vast, covering at least stand ∼1 km above the surrounding plain. The north- 540,000 km2, and its surface appears visually smoother ern margin shows a 2 km drop from Vulcan Planum, when compared to the heavily tectonized surface of Oz but the western margin only 1 km, and the south and Terra [1,2]. Vulcan Planum contains craters, rilles, east do not have a distinct lobate margin but appear to mountains, and other topographic features. It exhibits a smoothly grade out from the floor of the depression up to variety of textures: definitely a smooth, lobate texture, the plains. but also a ridged/lineated texture in places, and pitted textures in others (Figure2). A detailed map of features Margins: Everywhere along the south-facing bound- can be found in [4]. ary scarps of Oz Terra [5] which establish Vulcan Planum’s northern boundary, the surface of the planum is Rilles: Vulcan Planum is criss-crossed with a pattern depressed a kilometer or more in elevation within about of rilles [1,2] which range from less than a kilometer to 20 km of the boundary. 3 km in width, and about half a kilometer in depth. They can be a few kilometers or hundreds in length. The rilles Where Vulcan Planum meets the scarps of Oz Terra, show an arcuate or sinuous pattern. In some locations the Vulcan Planum units always appear to onlap the they display an en echelon pattern. Some of the larger scarps, implying that the Vulcan Planum surface was em- rilles have Y-shaped intersections. placed after the scarps had been formed. The larger rilles appear to preferentially parallel the In the portion of Vulcan Planum between Spock strike of the Vulcan Planum/Oz Terra boundary, which crater and where Serenity Chasma’s eastern end tran- parallels the dominant strike direction of nearby tectonic sitions from a graben to a south-facing scarp, there features in Oz Terra [5] and we will be performing a more is a well-resolved pattern of dense parallel rilles and detailed analysis of their strike. It isn’t clear if the align- ridges which parallel the boundary. This surface texture ment of these rilles indicates a formation contemporane- only appears away from the depressed margin where the ous with plains emplacement, or a process that occurred planum materials are presumably thicker. afterwards. Flow Features: We interpret the lobate, rounded fea- Mountains: [1] and [2] described Vulcan Planum’s tures on Vulcan Planum to be the result of flow emplace- mountains. There are two large solitary massifs (But- ment of the surface. The lobate margins which encir- ler and Kubrick Mons) and one cluster of three smaller cle the mountains appear to be the result of viscous flow peaks (Clarke Montes). Vulcan Planum does not onlap which has encountered an obstacle. The depressed mar- the toe of these mountains, but instead displays a con- gins along the Oz Terra scarps also imply a viscous flow, vex, depressed margin which surrounds them, engender- but the difference in width between the moats around ing the term ‘mountain in a moat’ for these features. the mountains and the depressed margin along the scarps Butler Mons is the largest, but by the time of closest may be due to the different depths of the viscous fluid approach it had set below the terminator. It can be seen in the center versus the potentially shallower depths at in approach images which show substantial scarps to its the margins. Further evidence for flow related to Vul- east and south which may indicate a hitherto unknown can Planum is a long tongue of smoother material which southern boundary to Vulcan Planum. stretches into Oz Terra north from Alice crater [5]. Lunar and Planetary Science XLVIII (2017) 2679.pdf Figure 1: LORRI mosaic of Charon’s Vulcan Planum. canically emplaced unit [1,2,6], similar to that seen on Ariel and Miranda [7] and other icy bodies in the solar system. The extent and age of resurfacing is comparable to that seen on saturnian and uranian satellites [6]. This work was supported by NASA’s New Horizons Project. References [1] S. A. Stern, et al. The Pluto system: Initial results from its exploration by New Horizons. Science, 350(6258), 2015. doi:10.1126/science.aad1815. [2] J. M. Moore, et al. The geology of Pluto and Charon through the eyes of New Horizons. Science, 351:1284– 1293, 2016. doi:10.1126/science.aad7055. [3] K. N. Singer, et al. Craters on Pluto and Charon – Surface Ages and Impactor Populations. In Lunar and Planetary Science Conference, volume 47, page 2310. 2016. [4] S. J. Robbins et al. Geologic map of New Horizons’ en- counter hemisphere of Charon, III. In Lunar and Planetary Science Conference, volume 48, page 1231. 2017. [5] Ross A. Beyer, et al. Charon tectonics. Icarus, 2016. ISSN Figure 2: Portion of PELR C MVIC LORRI CA at 0019-1035. doi:10.1016/j.icarus.2016.12.018. 157 m/pixel mosaic showing Vulcan Planum textures at [6] J. R. Spencer, et al. Geology and Composition of Pluto and the highest resolution. Charon from New Horizons. In AAS/Division for Planetary Sciences Meeting, volume 48, page 205.01. 2016. [7] D. G. Jankowski and S. W. Squyres. Solid-state ice volcan- ism on the satellites of Uranus. Science, 241:1322–1325, 1988. doi:10.1126/science.241.4871.1322. Conclusions: These observations of Vulcan Planum continue to support the conclusion that it is a cryovol-.
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