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Geological Mapping of Pluto and Charon using New Horizons data

Show simple item record Moore, J. (Jeff) Spencer, John R. (John Robert), 1957- McKinnon, William B. Howard, Alan D. White, Oliver L. Umurhan, Orkan M., 1969- Schenk, Paul M. Beyer, Ross A. Singer, Kelsi N. Stern, Alan, 1957- Weaver, Harold A., 1953- Young, Leslie A. Smith, K. Ennico Olkin, Cathy B. New Horizons Geology and Geophysics Imaging Team
dc.coverage.spatial Pluto (Dwarf planet)
dc.coverage.spatial Charon (Satellite) 2020-02-20T20:14:01Z 2020-02-20T20:14:01Z 2016
dc.identifier.citation Moore, J. M., Spencer, J. R., McKinnon, W. B., Howard, A. D., White, O. M., Umurhan, O. M., Schenk, P. M., Beyer, R. A., Singer, K., Stern, S. A., Weaver, H. A., Young, L. A., Ennico Smith, K., Olkin, C., and New Horizons Geology and Geophysics Imaging Team: GEOLOGICAL MAPPING OF PLUTO AND CHARON USING NEW HORIZONS DATA, Int. Arch. Photogramm. Remote Sens. Spatial Inf. Sci., XLI-B4, 449–451,, 2016. en
dc.identifier.other doi:10.5194/isprsarchives-XLI-B4-449-2016
dc.identifier.other (OCoLC)1151628536
dc.description.abstract Pluto and Charon exhibit strikingly different surface appearances, despite their similar densities and presumed bulk compositions. Systematic mapping has revealed that much of Pluto's surface can be attributed to surface-atmosphere interactions and the mobilization of volatile ices by insolation. Many mapped valley systems appear to be the consequence of glaciation involving nitrogen ice. Other geological activity requires or required internal heating. The convection and advection of volatile ices in Sputnik Planum can be powered by present-day radiogenic heat loss. On the other hand, the prominent mountains at the western margin of Sputnik Planum, and the strange, multi-km-high mound features to the south, probably composed of H2O, are young geologically as inferred by light cratering and superposition relationships. Their origin, and what drove their formation so late in Solar System history, is under investigation. The dynamic remolding of landscapes by volatile transport seen on Pluto is not unambiguously evident in the mapping of Charon. Charon does, however, display a large resurfaced plain and globally engirdling extensional tectonic network attesting to its early endogenic vigor. en
dc.description.statementofresponsibility J.M. Moore, J.R. Spencer, W.B. McKinnon, A.D. Howard, O.M. White, O.M. Umurhan, P.M. Schenk, R.A. Beyer, K. Singer, S.A. Stern, H.A. Weaver, L.A. Young, K. Ennico Smith, C. Olkin, and the New Horizons Geology and Geophysics Imaging Teamz
dc.format.extent Pages 449-451
dc.format.mimetype application/pdf
dc.language.iso en en
dc.publisher ISPRS en
dc.relation.ispartofseries LPI contribution ; no. 2272
dc.subject Pluto (Dwarf planet) en
dc.subject Charon (Satellite) en
dc.subject Geological mapping en
dc.title Geological Mapping of Pluto and Charon using New Horizons data en
dc.type Article en
dc.rights.license This work is distributed under the Creative Commons Attribution 3.0 License.

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