NASA Jet Propulsion Laboratory California Institute of Technology Follow this link to skip to the main content

BEACON eSpace at Jet Propulsion Laboratory >
JPL Technical Report Server >
JPL TRS 1992+ >

Please use this identifier to cite or link to this item: http://hdl.handle.net/2014/39224

Title: Geology of the Gusec cratered plains from the Spirit rover transverse
Authors: Golombek, M. P.
Crumpler, L. S.
Grant, J. A.
Greely, R.
Cabrol, N. A.
Parker, T. J.
Rice, J. W. Jr.
Ward, J. G.
Arvidson, R. E.
Moersch, J. E.
Fergason, J. F.
Christensen, P. R.
Castano, A.
Castano, R.
Haldemann, A. F. C.
Li, R.
Bell, J. F. III
Squyres, S. W.
Keywords: Gusev
Mars Exploration Rover (MER)
Spirit
Issue Date: 12-Jan-2006
Publisher: American Geophysical Union
Citation: Journal of Geophysical Research, Vol. 111, EO2S07
Abstract: The cratered plains of Gusev traversed by Spirit are generally low-relief rocky plains dominated by impact and eolian processes. Ubiquitous shallow, soil-filled, circular depressions, called hollows, are modified impact craters. Rocks are dark, fine-grained basalts, and the upper 10 m of the cratered plains appears to be an impact-generated regolith developed over intact basalt flows. Systematic field observations across the cratered plains identified vesicular clasts and rare scoria similar to original lava flow tops, consistent with an upper inflated surface of lava flows with adjacent collapse depressions. Crater and hollow morphometry are consistent with most being secondaries. The size frequency distribution of rocks >0.1 m diameter generally follows exponential functions similar to other landing sites for total rock abundances of 5–35%. Systematic clast counts show that areas with higher rock abundance and more large rocks have higher thermal inertia. Plains with lower thermal inertia have fewer rocks and substantially more pebbles that are well sorted and evenly spaced, similar to a desert pavement or lag. Eolian bed forms (ripples and wind tails) have coarse surface lags, and many are dust covered and thus likely inactive. Deflation of the surface _5–25 cm likely exposed two-toned rocks and elevated ventifacts and transported fines into craters creating the hollows. This observed redistribution yields extremely slow average erosion rates of _0.03 nm/yr and argues for very little long-term net change of the surface and a dry and desiccating environment similar to today’s since the Hesperian (or _3 Ga).
URI: http://hdl.handle.net/2014/39224
Appears in Collections:JPL TRS 1992+

Files in This Item:

File Description SizeFormat
05-2518.pdf2.26 MBAdobe PDFView/Open

Items in DSpace are protected by copyright, but are furnished with U.S. government purpose use rights.

 

Privacy/Copyright Image Policy Beacon Home Contact Us
NASA Home Page + Div 27
+ JPL Space
Site last updated on December 5, 2014.
If you have any comments or suggestions for this web site, please e-mail Robert Powers.