Overview of the Mars Pathfinder Mission: Launch through Landing, Surface Operations, Data Sets, and Science Results

Autor: Robert B. Hargraves, Jens Martin Knudsen, S.W. Thurman, William M. Folkner, G. R. Wilson, Scott L. Murchie, Pete Smith, Ralf Jaumann, Carol R. Stoker, R. M. Manning, Robert M. Haberle, R. L. Kirk, James R. Murphy, T.P. Rivellini, David Crisp, Heinrich Wänke, Thanasis E. Economou, Joy A. Crisp, John T. Schofield, Robert B. Singer, Mark T. Lemmon, Martin G. Tomasko, Nicolas Thomas, J.A. Magalhaes, K. E. Herkenhoff, Rudolf Rieder, J.A. Harris, Alvin Seiff, M. P. Golombek, Jeffrey R. Barnes, Jeffrey R. Johnson, Nathan T. Bridges, Michael C. Malin, James F. Bell, H. U. Keller, R. M. Vaughan, T. J. Parker, Søren Ejling Larsen, David A. Spencer, Ryan C. Sullivan, Albert F. C. Haldemann, Justin N. Maki, P. H. Kallemeyn, Daniel T. Britt, Ronald Greeley, Stubbe F. Hviid, Harry Y. McSween, J. Brückner, Jacob R. Matijevic, R. A. Cook, Morten Madsen, A. W. Ward, L. A. Soderblom, Robert C. Anderson, Henry J. Moore
Rok vydání: 1999
Předmět:
Zdroj: Scopus-Elsevier
Popis: 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 million individual temperature, pressure and wind measurements. Path-finder is the best known location on Mars, having been clearly identified with respect to other features on the surface by correlating five prominent horizon features and two small craters in lander images with those in high-resolution orbiter images and in inertial space from two-way ranging and Doppler tracking. Tracking of the lander has fixed the spin pole of Mars, determined the precession rate since Viking 20 years ago, and indicates a polar moment of inertia, which constrains a central metallic core to be between 1300 and ∼2000 km in radius. Dark rocks appear to be high in silica and geochemically similar to anorogenic andesites; lighter rocks are richer in sulfur and lower in silica, consistent with being coated with various amounts of dust. Rover and lander images show rocks with a variety of morphologies, fabrics and textures, suggesting a variety of rock types are present. Rounded pebbles and cobbles on the surface as well as rounded bumps and pits on some rocks indicate these rocks may be conglomerates (although other explanations are also possible), which almost definitely require liquid water to form and a warmer and wetter past. Air-borne dust is composed of composite silicate particles with a small fraction of a highly magnetic mineral, interpreted to be most likely maghemite; explanations suggest iron was dissolved from crustal materials during an active hydrologic cycle with maghemite freeze dried onto silicate dust grains. Remote sensing data at a scale of a kilometer or greater and an Earth analog correctly predicted a rocky plain safe for landing and roving with a variety of rocks deposited by catstrophic floods, which are relatively dust free. The surface appears to have changed little since it formed billions of years ago, with the exception that eolian activity may have deflated the surface by ∼3–7 cm, sculpted wind tails, collected sand into dunes, and eroded ventifacts (fluted and grooved rocks). Pathfinder found a dusty lower atmosphere, early morning water ice clouds, and morning near-surface air temperatures that changed abruptly with time and height. Small scale vortices, interpreted to be dust devils, were observed repeatedly in the afternoon by the meteorology instruments and have been imaged.
Databáze: OpenAIRE
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