HR: 10:50h
AN: P21C-03    [PDF]
TI: Physical Properties of the MER and Beagle II Landing Sites on Mars
AU: * Jakosky, B M
EM: bruce.jakosky@lasp.colorado.edu
AF: Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80309-0392 United States
AU: Pelkey, S M
AF: Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80309-0392 United States
AU: Mellon, M T
AF: Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80309-0392 United States
AU: Putzig, N
AF: Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80309-0392 United States
AU: Martinez-Alonso, S
AF: Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80309-0392 United States
AU: Murphy, N
AF: Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80309-0392 United States
AU: Hynek, B
AF: Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80309-0392 United States
AB: The ESA Beagle II and the NASA Mars Exploration Rover spacecraft are scheduled to land on the martian surface in December 2003 and January 2004, respectively. Mission operations and success depends on the physical properties of the surfaces on which they land. Surface structural characteristics such as the abundances of loose, unconsolidated fine material, of fine material that has been cemented into a duricrust, and of rocks affect the ability to safely land and to successfully sample and traverse the surface. Also, physical properties affect surface and atmospheric temperatures, which affect lander and rover functionality. We are in the process of analyzing surface temperature information for these sites, derived from MGS TES and Odyssey THEMIS daytime and nighttime measurements. Our approach is to: (i) remap thermal inertia using TES data at ~3-km resolution, to obtain the most complete coverage possible; (ii) interpret physical properties from TES coverage in conjunction with other remote-sensing data sets; (iii) map infrared brightness using daytime and nighttime THEMIS data at 100-m resolution, and do qualitative analysis of physical properties and processes; and (iv) derive thermal inertia from THEMIS nighttime data in conjunction with daytime albedo measurements derived from TES, THEMIS, and MOC observations. In addition, we will use measured temperatures and derived thermal inertia to predict surface temperatures for the periods of the missions.
DE: 6225 Mars
SC: Planetary Sciences [P]
MN: 2003 Fall Meeting