Publications
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Variability of Mars' North Polar water ice cap: I. Analysis of Mariner 9 and Viking Orbiter imaging data
Previous studies interpreted differences in ice coverage between Mariner 9 and Viking Orbiter observations of Mars' north residual polar cap as evidence of interannual variability of ice deposition on the cap. However, these investigators did not consider the possibility that there could be significant changes in the ice coverage within the northern residual cap over the course of the summer seaso
Authors
Deborah S. Bass, Kenneth E. Herkenhoff, David A. Paige
Surface properties of Mars' polar layered deposits and polar landing sites
On December 3, 1999, the Mars Polar Lander and Mars Microprobes will land on the planet's south polar layered deposits near (76°S, 195°W) and conduct the first in situ studies of the planet's polar regions. The scientific goals of these missions address several poorly understood and globally significant issues, such as polar meteorology, the composition and volatile content of the layered deposits
Authors
Ashwin R. Vasavada, Jean-Pierre Williams, David A. Paige, Kenneth E. Herkenhoff, Nathan T. Bridges, Ronald Greeley, Bruce C. Murray, Deborah S. Bass, Karen S. McBride
Sinus Meridiani: uncontrolled Mars Global Surveyor (MGS) Mars Orbital Camera (MOC): digital context photomosaic (250 megapixel resolution)
These images were processed from a raw format using Integrated Software for Images and Spectrometers (ISIS) to perform radiometric corrections and projection. All the images were projected in sinusoidal using a center longitude of 0 degrees. There are two versions of the mosaic, one unfiltered (sinusmos.tif), and one produced with all images processed through a box filter with an averaged pixel to
Authors
Eric Noreen
Central Valles Marineris: uncontrolled Mars Global Surveyor (MGS) Mars Orbital Camera (MOC) digital context photomosaic (250 megapixel resolution)
These images were processed from a raw format using Integrated Software for Images and Spectrometers (ISIS) to perform radiometric corrections and projection. All the images were projected in sinusoidal using a center longitude of 70 degrees. There are two versions of the mosaic, one unfiltered (vallesmos.tif), and one produced with all images processed through a box filter with an averaged pixel
Authors
Eric Noreen
Does Europa have a subsurface ocean? Evaluation of the geological evidence
It has been proposed that Jupiter's satellite Europa currently possesses a global subsurface ocean of liquid water. Galileo gravity data verify that the satellite is differentiated into an outer H2O layer about 100 km thick but cannot determine the current physical state of this layer (liquid or solid). Here we summarize the geological evidence regarding an extant subsurface ocean, concentrating o
Authors
Robert T. Pappalardo, Michael J.S. Belton, H.H. Breneman, M. H. Carr, Clark R. Chapman, G.C. Collins, T. Denk, S. Fagents, Paul E. Geissler, B. Giese, R. Greeley, R. Greenberg, J.W. Head, P. Helfenstein, G. Hoppa, S.D. Kadel, K.P. Klaasen, James E. Klemaszewski, K.P. Magee, Alfred S. McEwen, J.M. Moore, W.B. Moore, G. Neukum, C.B. Phillips, L.M. Prockter, G. Schubert, D.A. Senske, R.J. Sullivan, B.R. Tufts, E. P. Turtle, Robert Wagner, K.K. Williams
Observations of Phobos, Deimos, and bright stars with the Imager for Mars Pathfinder
The Imager for Mars Pathfinder (IMP) was used to observe several objects during the Martian night. The satellites, Phobos and Deimos, were observed on two occasions each, through the IMP geological filters covering the wavelength range 440 nm to 1 μm. The observations were converted to geometric albedo using triaxial ellipsoid models of the satellites and phase functions derived from Viking Orbite
Authors
Nick Thomas, D.T. Britt, Kenneth E. Herkenhoff, Scott L. Murchie, B. Semenov, H.U. Keller, P. H. Smith
Mars Pathfinder spectral measurements of Phobos and Deimos: Comparison with previous data
The Imager for Mars Pathfinder (IMP) acquired four spectra of parts of the sub‐Mars hemispheres of Phobos and Deimos. The measured region of Phobos is expected to be a mixture of the two spectral units identified on that satellite from Phobos 2 data, and the IMP spectra of Phobos are intermediate to the two units as expected. The derived geometric albedo is consistent with the value for that part
Authors
Scott L. Murchie, Nick Thomas, Daniel Britt, Kenneth E. Herkenhoff, James F. Bell
Overview of the Mars Pathfinder Mission: Launch through landing, surface operations, data sets, and science results
Mars Pathfinder successfully landed at Ares Vallis on July 4, 1997, deployed and navigated a small rover about 100 m clockwise around the lander, and collected data from three science instruments and ten technology experiments. The mission operated for three months and returned 2.3 Gbits of data, including over 16,500 lander and 550 rover images, 16 chemical analyses of rocks and soil, and 8.5 mil
Authors
M. P. Golombek, R. C. Anderson, J.R. Barnes, J. F. III Bell, N. T. Bridges, D.T. Britt, J. Brückner, R. A. Cook, D. Crisp, J.A. Crisp, T. Economou, W. M. Folkner, R. Greeley, R.M. Haberle, R.B. Hargraves, J.A. Harris, A. F. C. Haldemann, Kenneth E. Herkenhoff, S.F. Hviid, R. Jaumann, J. R. Johnson, P. H. Kallemeyn, H.U. Keller, Randolph L. Kirk, J. M. Knudsen, S. Larsen, M. T. Lemmon, M.B. Madsen, J.A. Magalhães, J.N. Maki, M.C. Malin, R. M. Manning, J. Matijevic, H.Y. McSween, H. J. Moore, S.L. Murchie, J.R. Murphy, T. J. Parker, R. Rieder, T.P. Rivellini, J. T. Schofield, A. Seiff, R.B. Singer, P. H. Smith, Laurence A. Soderblom, D.A. Spencer, C. R. Stoker, R. Sullivan, N. Thomas, S.W. Thurman, M.G. Tomasko, R. M. Vaughan, H. Wänke, A. W. Ward, G.R. Wilson
General geology and geomorphology of the Mars Pathfinder landing site
The Mars Pathfinder (MPF) spacecraft landed on relatively young (late Hesperian-early Amazonian; 3.1-0.7 Ga) plains in Chryse Planitia near the mouth of Ares Vallis. Images returned from the spacecraft reveal a complex landscape of ridges and troughs, large hills and crater rims, rocks and boulders of various sizes and shapes, and surficial deposits, indicating a complex, multistage geologic histo
Authors
A. W. Ward, Lisa R. Gaddis, Randolph L. Kirk, Laurence A. Soderblom, K. L. Tanaka, M.P. Golombek, T. J. Parker, Ronald Greeley, R.O. Kuzmin
Digital photogrammetric analysis of the IMP camera images: Mapping the Mars Pathfinder landing site in three dimensions
This paper describes our photogrammetric analysis of the Imager for Mars Pathfinder data, part of a broader program of mapping the Mars Pathfinder landing site in support of geoscience investigations. This analysis, carried out primarily with a commercial digital photogrammetric system, supported by our in‐house Integrated Software for Imagers and Spectrometers (ISIS), consists of three steps: (1)
Authors
Randolph L. Kirk, Elpitha Howington-Kraus, Trent M. Hare, E. Dorrer, D. Cook, Kris J. Becker, K. Thompson, B. Redding, J. Blue, D. Galuszka, E.M. Lee, Lisa R. Gaddis, J. R. Johnson, Laurence A. Soderblom, A. W. Ward, P. H. Smith, D.T. Britt
Digital mapping of the Mars Pathfinder landing site: Design, acquisition, and derivation of cartographic products for science applications
The Imager for Mars Pathfinder (IMP) acquired more than 16,000 images and provided panoramic views of the surface of Mars at the Mars Pathfinder landing site in Ares Vallis. This paper describes the stereoscopic, multispectral IMP imaging sequences and focuses on their use for digital mapping of the landing site and for deriving cartographic products to support science applications of these data.
Authors
Lisa R. Gaddis, Randolph L. Kirk, J. R. Johnson, Laurence A. Soderblom, A. W. Ward, J. Barrett, Kris J. Becker, Tammy L. Becker, J. Blue, D. Cook, E. Eliason, Trent M. Hare, Elpitha Howington-Kraus, C. Isbell, E.M. Lee, Bonnie L. Redding, Robert M. Sucharski, Tracie L. Sucharski, P. H. Smith, D.T. Britt
Geology of the Upheaval Dome impact structure, southeast Utah
Two vastly different phenomena, impact and salt diapirism, have been proposed for the origin of Upheaval Dome, a spectacular scenic feature in southeast Utah. Detailed geologic mapping and seismic refraction data indicate that the dome originated by collapse of a transient cavity formed by impact. Evidence is as follows: (1) sedimentary strata in the center of the structure are pervasively imbrica
Authors
Bryan J. Kriens, Eugene M. Shoemaker, Kenneth E. Herkenhoff