Some Geologic Problems of Mars

Research Article| October 01, 1965 Some Geologic Problems of Mars ALDEN A LOOMIS ALDEN A LOOMIS Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California Search for other works by this author on: GSW Google Scholar Author and Article Information ALDEN A LOOMIS Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California Publisher: Geological Society of America Received: 02 Feb 1965 First Online: 02 Mar 2017 Online ISSN: 1943-2674 Print ISSN: 0016-7606 Copyright © 1965, The Geological Society of America, Inc. Copyright is not claimed on any material prepared by U.S. government employees within the scope of their employment. GSA Bulletin (1965) 76 (10): 1083–1104. https://doi.org/10.1130/0016-7606(1965)76[1083:SGPOM]2.0.CO;2 Article history Received: 02 Feb 1965 First Online: 02 Mar 2017 Cite View This Citation Add to Citation Manager Share Icon Share Facebook Twitter LinkedIn Email Permissions Search Site Citation ALDEN A LOOMIS; Some Geologic Problems of Mars. GSA Bulletin 1965;; 76 (10): 1083–1104. doi: https://doi.org/10.1130/0016-7606(1965)76[1083:SGPOM]2.0.CO;2 Download citation file: Ris (Zotero) Refmanager EasyBib Bookends Mendeley Papers EndNote RefWorks BibTex toolbar search Search Dropdown Menu toolbar search search input Search input auto suggest filter your search All ContentBy SocietyGSA Bulletin Search Advanced Search Abstract Data on the body of Mars are as yet insufficient to allow computation of meaningful models of the internal structure or density stratification within the planet. The flattening of the solid surface appears to be greater than the flattening of the equipotential surface by about a factor of two. The resultant possibility that the equatorial regions are high compared to the polar areas has many geological and biological implications.Most of the inner planets—Mercury, Venus, Earth, Moon, and Mars—have bulk compositions which differ from one another as well as from that of the stony meteorites. The thermal histories of the planets have therefore differed because of different original compositions as well as different sizes and distances from the Sun.More data on the surface topography are required in order to make geological interpretations which are not largely subjective. The dark areas could be either highlands or lowlands relative to surrounding bright areas. Although sharp relief of several thousand feet is probably absent or nearly so, substantial mountain ranges, plateaus, or basins could exist if the slopes on their flanks are gradual. Liquid water cannot exist on the surface of Mars, and aqueous erosion features, if they once existed, have become subdued by aeolian activity.Winds on Mars may move more and coarser material than winds on Earth. Deep accumulations of aeolian deposits have formed, at least locally. Mariner IV pictures show an impact-crater distribution much like the highland areas of the Moon. Many craters with original depths of less than about 8000–10,000 feet have become obliterated on Mars by windblown dust. This content is PDF only. Please click on the PDF icon to access. First Page Preview Close Modal You do not have access to this content, please speak to your institutional administrator if you feel you should have access.