-
P H Smith,
J F Bell,
N T Bridges,
D T Britt,
L Gaddis,
R Greeley,
H U Keller,
K E Herkenhoff,
R Jaumann,
J R Johnson, [......],
J Oberst,
T J Parker,
R J Reid,
R Sablotny,
L A Soderblom,
C Stoker,
R Sullivan,
N Thomas,
M G Tomasko, E Wegryn
[show abstract]
[hide abstract]
ABSTRACT: Images of the martian surface returned by the Imager for Mars Pathfinder (IMP) show a complex surface of ridges and troughs covered by rocks that have been transported and modified by fluvial, aeolian, and impact processes. Analysis of the spectral signatures in the scene (at 440- to 1000-nanometer wavelength) reveal three types of rock and four classes of soil. Upward-looking IMP images of the predawn sky show thin, bluish clouds that probably represent water ice forming on local atmospheric haze (opacity approximately 0.5). Haze particles are about 1 micrometer in radius and the water vapor column abundance is about 10 precipitable micrometers.
Science 01/1998; 278(5344):1758-65. · 31.20 Impact Factor
-
R.J. Reid,
P.H. Smith,
M. Lemmon,
R. Tanner,
M. Burkland, E. Wegryn,
J. Weinberg,
R. Marcialis,
N. Thomas,
R. Kramm,
A. Dummel,
D. Crowe,
B.J. Bos,
P. Rueffer,
F. Gliem,
J.R. Johnson,
J.N. Maki,
K.E. Herkenhoff
Journal of Geophysical Research. 104(1999-E4).
-
P.H. Smith,
J.F. Bell,
N.T. Bridges,
D.T. Britt,
L. Gaddis,
R. Greeley,
H.U. Keller,
K.E. Herkenhoff,
R. Jaumann,
J.R. Johnson, [......],
T.J. Parker,
R.J. Reid,
R. Sablotny,
L.A. Soderblom,
C. Stoker,
R. Sullivan,
N. Thomas,
M.G. Tomasko,
W. Ward, E. Wegryn
Science. 278(1997):1758-1764.
