Abstract
The age relations between 36 impact craters with dark paraboloids and other geologic units and structures at these localities have been studied through photogeologic analysis of Magellan SAR images of the surface of Venus. Geologic settings in all 36 sites, about 1000 × 1000 km each, could be characterized using only 10 different terrain units and six types of structures. These units and structures form a major stratigraphic and geologic sequence (from oldest to youngest): 1) tessera terrain; 2) densely fractured terrains associated with coronae and in the form of remnants among plains; 3) fractured and ridged plains and ridge belts; 4) plains with wrinkle ridges; 5) ridges associated with coronae annulae and ridges of arachnoid annulae which are contemporary with wrinkle ridges of the ridged plains; 6) smooth and lobate plains; 7) fractures of coronae annulae, and fractures not related to coronae annulae, which disrupt ridged and smooth plains; 8) rift-associated fractures; 9) craters with associated dark paraboloids, which represent the youngest 10% of the Venus impact crater population (Campbellet al., 1992), and are on top of all volcanic and tectonic units except the youngest episodes of rift-associated fracturing and volcanism; surficial streaks and patches are approximately contemporary with dark-paraboloid craters.
Mapping of such units and structures in 36 randomly distributed large regions (each ∼ 106 km2) shows evidence for a distinctive regional and global stratigraphic and geologic sequence. On the basis of this sequence we have developed a model that illustrates several major themes in the history of Venus. Most of the history of Venus (that of its first 80% or so) is not preserved in the surface geomorphological record. The major deformation associated with tessera formation in the period sometime between 0.5–1.0 b.y. ago (Ivanov and Basilevsky, 1993) is the earliest event detected. In the terminal stages of tessera formation, extensive parallel linear graben swarms representing a change in the style of deformation from shortening to extension were formed on the tessera and on some volcanic plains that were emplaced just after (and perhaps also during the latter stages of the major compressional phase of tessera emplacement. Our stratigraphic analyses suggest that following tessera formation, extensive volcanic flooding resurfaced at least 85% of the planet in the form of the presently-ridged and fractured plains. Several lines of evidence favor a high flux in the post-tessera period but we have no independent evidence for the absolute duration of ridged plains emplacement. During this time, the net state of stress in the lithosphere apparently changed from extensional to compressional, first in the form of extensive ridge belt development, followed by the formation of extensive wrinkle ridges on the flow units. Subsequently, there occurred local emplacement of smooth and lobate plains units which are presently essentially undeformed. The major events in the latest 10% of the presently preserved history of Venus (less than 50 m.y. ago) are continued rifting and some associated volcanism, and the redistribution of eolian material largely derived from impact crater deposits.
Detailed geologic mapping and stratigraphic synthesis are necessary to test this sequence and to address many of the outstanding problems raised by this analysis. For example, we are uncertain whether this stratigraphic sequence corresponds to geologic events which were generally synchronous in all the sites and all around the planet, or whether the sequence is simply a typical sequence of events which occurred in different places at different times. In addition, it is currently unknown whether the present state represents a normal consequence of the general thermal evolution of Venus (and is thus representative of the level of geological activity predicted for the future), or if Venus, has been characterized by a sequence of periodic global changes in the composition and thermal state of its crust and upper mantle (in which case, Venus could in the future return to levels of deformation and resurfacing typical of the period of tessera formation).
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References
ACSN, 1961, American Code of Stratigraphic Nomenclature,Am. Assn. Petrol. Geol. Bull. 45, 645–660.
Barsukov, V. L.,et al.: 1986, ‘The Geology and Geomorphology of the Venus Surface as Revealed by the Radar Images Obtained by Venera 15 and 16’,J. Geophys. Res. 91, D399–411.
Basilevsky, A. T.: 1993, ‘Age of Rifting and Associated Volcanism in Atla, Regio, Venus’,Geophys. Res. Lett. 20, 883–886.
Basilevsky, A. T. and Head, J. W.: 1994, ‘Characteristics of the Geology of Thirty-Six Sites on Venus’, Brown University Library, Providence RI, 72 p.
Basilevsky, A. T., Pronin, A. A., Ronca, L. B., Kryuchkov, V. P., Sukhanov, A. L., and Markov, M. S.: 1986, ‘Styles of Tectonic Deformations on Venus: Analysis of Venera 15 and 16 Data’,J. Geophys. Res. 91, suppl., D399-D411.
Bilotti, F.: 1992, ‘Global Organization of Tectonic Deformation on Venus’,Lunar Planet. Sci. Conf. 24, 107–108.
Bindschadler, D. L. and Head, J. W.: 1991, ‘Tessera Terrain, Venus: Characterization and Models for Origin and Evolution’,J. Geophys. Res. 96(B4), 5889–5907.
Bindschadler, D. L., Schubert, G., and Kaula, W. M.: 1992, ‘Coldspots and Hotspots: Global Tectonic and Mantle Dynamics of Venus’,J. Geophys. Res. 97(E8), 13563–13578.
Bullock, M. A., Grinspoon, D. H., and Head, J. W.: 1993, ‘Venus Resurfacing Rates: Constraints Provided by 3-D Monte Carlo Simulations’,Geophys. Res. Lett. 20, 2147–2150.
Campbell, D. B., Stacy, N. J. S., Newman, W. I., Arvidson, R. E., Jones, E. M., Musser, G. S., Roper, A. Y., and Schaller, C.: 1992, ‘Magellan Observations of Extended Impact Crater Related Features on the Surface of Venus’,J. Geophys. Res. 97, 16249–16277.
Crumpler, L. S., Head, J. W., and Aubele, J. C.: 1993, ‘Relation of Major Volcanic Center Concentration on Venus to Global Tectonic Patterns’,Science 261, 591–595.
Diggle, P. J., Fisher, N. L, and Lee, A. J.: 1985, ‘A Comparison of Tests of Uniformity for Spherical Data’,Austral. J. Statistics 27, 53–59.
Greeley, R., Arvidson, R. E., Elachi, C., Geringer, M. A., Plaut, J. J., Saunders, R. S., Schubert, G., Stofan, E. R., Thouvenot, E. J. P., Wall, S. D., and Weitz, C. M.: 1992, ‘Aeolian Features on Venus: Preliminary Magellan Results’,J. Geophys. Res. 97(E8), 13319–13345.
Greeley, R. and Guest, J. E.: 1987,Geological Map of the Eastern Equatorial Region of Mars, U.S. Geological Survey Map I-1802-B.
Head, J. W., Crumpler, L. S., Aubele, J. C., Guest, J. E., and Saunders, R. S.: 1992, ‘Venus Volcanism: Classification of Volcanic Features and Structures, Associations, and Global Distribution from Magellan Data’,J. Geophys. Res. 97(E8), 13153–13197.
Head, J. W., Parmentier, E. M., and Hess, P. C.: 1994, ‘Venus: Vertical Accretion of Crust and Depleted Mantle and Implications for Geological History and Processes’,Planetary and Space Science, in press.
Head, J. W., Pieters, C. M., McCord, T. B., Adams, J. A., and Zisk, S.: 1978, ‘Definition and Detailed Characterization of Lunar Surface Units Using Remote Observations’,Icarus 33, 145–172.
Ivanov, M. A. and Basilevsky, A. T.: 1993, ‘Density and Morphology of Impact Craters on Tessera Terrain, Venus’,Geophys. Res. Lett. 20, 2579–2582.
Ivanov, M. A. and Head, J. W.: 1994, ‘Tessera Terrain on Venus: A Survey of the Global Distribution, Characteristics, and Relation to Surrounding Units from Magellan Data’,Earth, Moon and Planets, submitted.
McGill, G. E.: 1993, ‘Wrinkle Ridges, Stress Domains, and Kinematics of Venusian Plains’,Geophys. Res. Lett. 20, 2407–2410.
Nikishin, A. M., Pronin, A. A., and Basilevsky, A. T.: 1992, in V. L. Barsukovet al. (eds.),Hot-Spot Structures, in Venus Geology, Geochemistry, and Geophysics, Research Results from the USSR, University of Arizona Press, pp. 31–67.
Parmentier, E. M. and Hess, P. C.: 1992, ‘Chemical Differentiation of a Convecting Planetary Interior: Consequences for a One Plate Planet Such as Venus’,Geophys. Res. Lett. 19, 2015–2018.
Phillips, R., Raubertas, R. F., Arvidson, R. E., Sarkar, I. C., Herrick, R. R., Izenberg, N., and Grimm, R. E.: 1992, ‘Impact Craters and Venus Resurfacing History’,J. Geophys. Res. 97, 15923–15948.
Plaut, J.J.: 1993, in J. P. Fordet al. (eds.),Stereo Imaging, in Guide to Magellan Image Interpretation, Chapter 4, JPL Pub., 93–24, 33–44.
Roberts, K. M., Guest, J. E., Head, J. W., and Lancaster, M. G.: 1992, ‘Mylitta Fluctus, Venus: Rift-Related, Centralized Volcanism and the Emplacement of Large-Volume Flow Units’,J. Geophys. Res. 97, 15991–16015.
Schaber, G. G., Strom, R. G., Moore, H. J., Soderblom, L. A., Kirk, R. L., Chadwick, D. J., Dawson, D. D., Gaddis, L. R., Boyce, J. M., and Russell, J.: 1992, ‘Geology and Distribution of Impact Craters on Venus: What are They Telling Us?’,J. Geophys. Res. 97(E8), 13256–13302.
Scott, D. H. and Tanaka, K. L.: 1986, ‘Geological Map of the Western Equatorial Region of Mars’, U.S. Geological Survey Map I-1802-A.
Senske, D. A., Schaber, G. G., and Stofan, E. R.: 1992, ‘Regional Topographic Rises on Venus: Geology of Western Eistla Regio and Comparison to Beta Regio and Atla Regio’,J. Geophys. Res. 97, 13395–13420.
Squyres, S. W., Jankowski, D. G., Simons, M., Solomon, S. C., Hager, B. H., and McGill, G. E.: 1992, ‘Plains Tectonism on Venus: The Deformation Belts of Lavinia Planitia’,J. Geophys. Res. 97(E8), 13579–13599.
Solomon, S. C.: 1978, ‘On Volcanism and Thermal Tectonics on One-Plate Planets’,Geophys. Res. Lett. 5, 461–464.
Solomon, S. C.: 1993, ‘A Tectonic Resurfacing Model for Venus’,Lunar and Planetary Science Conference 24, 1331–1332.
Solomon, S. C. and Head, J. W.: 1980, ‘Lunar Mascon Basins: Lava Filling, Tectonics and Evolution of the Lithosphere’,Reviews of Geophysics and Space Physics 18, 107–141.
Solomon, S. C., Smrekar, S. C., Bindschadler, D. L., Grimm, R. E., Kaula, W. K., McGill, G. E., Phillips, R. J., Saunders, R. S., Schaber, G., Squyres, S. W., and Stofan, E. R.: 1992, ‘Venus Tectonics: An Overview of Magellan Observations’,J. Geophys. Res. 97, 13199–13255.
Stofan, E. R., Sharpton, V. L., Schubert, G., Baer, G., Bindschadler, D. L., Janes, D. M., and Squyres, S. W.: 1992, ‘Global Distribution and Characteristics of Coronae and Related Features on Venus: Implications for Origin and Relation to Mantle Processes’,J. Geophys. Res. 97(E8), 13347–13378.
Strom, R. G.: 1993, ‘Parabolic Features and the Erosion Rate on Venus’,Lunar and Planetary Science Conference 24, 1371–1372.
Strom, R. G., Schaber, G. G., and Dawson, D. D.: 1994, ‘The Global Resurfacing of Venus’,J. Geophys. Res. 99, 10899–10926.
Sukhanov, A. L.: 1992, in V. L. Barsukovet al. (eds.),Tesserae, in Venus Geology, Geochemistry, and Geophysics, Research Results from the USSR, University of Arizona Press, pp. 82–95.
Tanaka, K. L., (compiler): 1994,Venus Geologic Mappers' Handbook, Second Edition, U.S. Geological Survey Open File Report 94-438, 50 pp.
Tanaka, K. L. and Scott, D. H.: 1987,Geological Map of the Polar Regions of Mars, U.S. Geological Survey Map I-1802-C.
Weitz, C. M., Elachi, C., Moore, H. J., Basilevsky, A. T., Ivanov, B. A., and Schaber, G. G.: 1992, ‘Low Emissivity Impact Craters on Venus’,Int. Coll. on Venus, LPI Pub. 789, 129–131.
Wilhelms, D. E.: 1972,Geologic Mapping of the Second Planet, USGS Interagency Report 55, 36 PP.
Wilhelms, D. E.: 1990, in R. Greeley and R. M. Batson (eds.),Geologic Mapping, in Planetary Mapping, Cambridge University Press, New York, pp. 208–260.
Zuber, M. T. and Parmentier, E. M.: 1990, ‘On the Relationship between Isostatic Elevation and the Wavelengths of Tectonic Surface Features on Venus’,Icarus 85, 290–308.
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Basilevsky, A.T., Head, J.W. Global stratigraphy of Venus: analysis of a random. Earth Moon Planet 66, 285–336 (1994). https://doi.org/10.1007/BF00579467
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DOI: https://doi.org/10.1007/BF00579467