Ancient lowlands on Mars

[1] Mars Orbiter Laser Altimeter (MOLA) data provide compelling evidence that the martian lowlands, below the smooth and sparsely cratered northern plains, are extremely old, far older than the plains which cover them. The evidence is in the form of a very large population of “Quasi-Circular Depressions” (QCDs), many of which are very evident in the MOLA elevation data but generally not visible in available imagery. We interpret these “invisible” QCDs to be buried impact basins. Cumulative number versus diameter curves for lowland QCDs suggests the buried lowland surface is older than the visible highland surface and that the lowland plains are a relatively thin (1–2 km) veneer overlying this much older surface. We conclude that the martian lowlands have been low and stable for nearly all of martian history.

[1]  H. Frey,et al.  A Very Large Population of Likely Buried Impact Basins in the Northern Lowlands of Mars Revealed by MOLA Data , 2001 .

[2]  M. Zuber,et al.  Degree-1 mantle convection and the crustal dichotomy on Mars , 2000 .

[3]  A. Albee,et al.  Mars global surveyor mission: overview and status. , 1998, Science.

[4]  David E. Smith,et al.  The global topography of Mars and implications for surface evolution. , 1999, Science.

[5]  A Large Population of Possible Buried Impact Basins on Mars Revealed by MOLA Topographic Data , 2000 .

[6]  Geometry of maps between generalized flag manifolds , 1987 .

[7]  G. Mcgill.  Buried topography of Utopia, Mars: Persistence of a giant impact depression , 1989 .

[8]  J. H. Roark,et al.  GRIDVIEW: Recent Improvements in Research and Education Software for Exploring Mars Topography , 2001 .

[9]  T. Parker,et al.  The Evolution of the Martian Hydrosphere: Implications for the Fate of a Primordial Ocean and the Current State of the Northern Plains , 2001 .

[10]  H. Frey,et al.  A new survey of multiring impact basins on Mars , 1990 .

[11]  N. Sleep.  Martian plate tectonics , 1994 .

[12]  Norman H. Sleep,et al.  Evolution of the mode of convection within terrestrial planets , 2000 .

[13]  Richard A. Schultz,et al.  Large impact basins and the mega-impact origin for the crustal dichotomy on Mars , 1988 .

[14]  George E. McGill,et al.  Origin of the Martian global dichotomy by crustal thinning in the late Noachian or early Hesperian , 1990 .

[15]  Kenneth L. Tanaka.  The stratigraphy of Mars , 1986 .

[16]  H. Frey,et al.  Discovery of a 450 km diameter, multi‐ring basin on Mars through analysis of MOLA topographic data , 1999 .

[17]  K. Tanaka.  The stratigraphy of Mars.Proc.Lunar Planet.Sci.Conf.17 , 1986 .

[18]  M. Golombek,et al.  Tectonic evolution of Mars , 1979 .

[19]  Ronald Greeley,et al.  The resurfacing history of Mars - A synthesis of digitized, viking-based geology , 1988 .

[20]  James H. Roark,et al.  Interactive Graphics Tools for Analysis of MOLA and Other Data , 2000 .

[21]  R. Phillips,et al.  Evidence for extensive denudation of the Martian highlands , 2001 .

[22]  Richard A. Schultz,et al.  Speculations on the origin and evolution of the Utopia-Elysium lowlands of Mars , 1990 .

[23]  James B. Garvin,et al.  North Polar Region Craterforms on Mars: Geometric Characteristics from the Mars Orbiter Laser Altimeter , 2000 .