[1] The HiRISE camera features a 0.5 m diameter primary mirror, 12 m effective focal length, and a focal plane system that can acquire images containing up to 28 Gb (gigabits) of data in as little as 6 seconds. HiRISE will provide detailed images (0.25 to 1.3 m/pixel) covering ∼1% of the Martian surface during the 2-year Primary Science Phase (PSP) beginning November 2006. Most images will include color data covering 20% of the potential field of view. A top priority is to acquire ∼1000 stereo pairs and apply precision geometric corrections to enable topographic measurements to better than 25 cm vertical precision. We expect to return more than 12 Tb of HiRISE data during the 2-year PSP, and use pixel binning, conversion from 14 to 8 bit values, and a lossless compression system to increase coverage. HiRISE images are acquired via 14 CCD detectors, each with 2 output channels, and with multiple choices for pixel binning and number of Time Delay and Integration lines. HiRISE will support Mars exploration by locating and characterizing past, present, and future landing sites, unsuccessful landing sites, and past and potentially future rover traverses. We will investigate cratering, volcanism, tectonism, hydrology, sedimentary processes, stratigraphy, aeolian processes, mass wasting, landscape evolution, seasonal processes, climate change, spectrophotometry, glacial and periglacial processes, polar geology, and regolith properties. An Internet Web site (HiWeb) will enable anyone in the world to suggest HiRISE targets on Mars and to easily locate, view, and download HiRISE data products.

/pdf/mars-reconnaissance-orbiter-s-high-resolution-imaging-4bjw0ks5y9.pdf

Mars Reconnaissance Orbiter's High Resolution Imaging Science Experiment (HiRISE)

The Mars Orbiter Laser Altimeter (MOLA), an instrument on the Mars Global Surveyor spacecraft, has measured the topography, surface roughness, and 1.064-μm reflectivity of Mars and the heights of volatile and dust clouds. This paper discusses the function of the MOLA instrument and the acquisition, processing, and correction of observations to produce global data sets. The altimeter measurements have been converted to both gridded and spherical harmonic models for the topography and shape of Mars that have vertical and radial accuracies of ~1 m with respect to the planet's center of mass. The current global topographic grid has a resolution of 1/64° in latitude × 1/32° in longitude (1 × 2 km^2 at the equator). Reconstruction of the locations of incident laser pulses on the Martian surface appears to be at the 100-m spatial accuracy level and results in 2 orders of magnitude improvement in the global geodetic grid of Mars. Global maps of optical pulse width indicative of 100-m-scale surface roughness and 1.064-μm reflectivity with an accuracy of 5% have also been obtained.

/pdf/mars-orbiter-laser-altimeter-experiment-summary-after-the-3w1byzpn90.pdf

Mars Orbiter Laser Altimeter: Experiment summary after the first year of global mapping of Mars

The composition of the primitive mantle derived here shows that Earth was assembled from material that shows many of the same chemical fractionation processes as chondritic meteorites. These processes occurred at the initial stage of the solar system formation, under conditions thought to be present in the solar nebula. But the stable isotope record excludes chondritic meteorites as the ‘building blocks’ of Earth. Meteorites formed in local environments separated from that part of the inner solar system where much of the material forming the terrestrial planets was sourced.

https://booksite.elsevier.com/brochures/treatiseongeochemistry/contents/sample2.pdf

Cosmochemical Estimates of Mantle Composition

Jupiter and Saturn formed in a few million years from a gas-dominated protoplanetary disk, and were susceptible to gas-driven migration of their orbits on timescales of only approximately 100,000 years. Hydrodynamic simulations show that these giant planets can undergo a two-stage, inward-then-outward, migration. The terrestrial planets finished accreting much later and their characteristics, including Mars' small mass, are best reproduced by starting from a planetesimal disk with an outer edge at about one astronomical unit from the Sun (1 AU is the Earth-Sun distance). Here we report simulations of the early Solar System that show how the inward migration of Jupiter to 1.5 AU, and its subsequent outward migration, lead to a planetesimal disk truncated at 1 AU; the terrestrial planets then form from this disk over the next 30-50 million years, with an Earth/Mars mass ratio consistent with observations. Scattering by Jupiter initially empties but then repopulates the asteroid belt, with inner-belt bodies originating between 1 and 3 AU and outer-belt bodies originating between and beyond the giant planets. This explains the significant compositional differences across the asteroid belt. The key aspect missing from previous models of terrestrial planet formation is the substantial radial migration of the giant planets, which suggests that their behaviour is more similar to that inferred for extrasolar planets than previously thought.

A low mass for Mars from Jupiter's early gas―driven migration

[1] The Context Camera (CTX) on the Mars Reconnaissance Orbiter (MRO) is a Facility Instrument (i.e., government-furnished equipment operated by a science team not responsible for design and fabrication) designed, built, and operated by Malin Space Science Systems and the MRO Mars Color Imager team (MARCI). CTX will (1) provide context images for data acquired by other MRO instruments, (2) observe features of interest to NASA's Mars Exploration Program (e.g., candidate landing sites), and (3) conduct a scientific investigation, led by the MARCI team, of geologic, geomorphic, and meteorological processes on Mars. CTX consists of a digital electronics assembly; a 350 mm f/3.25 Schmidt-type telescope of catadioptric optical design with a 5.7° field of view, providing a ∼30-km-wide swath from ∼290 km altitude; and a 5000-element CCD with a band pass of 500–700 nm and 7 μm pixels, giving ∼6 m/pixel spatial resolution from MRO's nearly circular, nearly polar mapping orbit. Raw data are transferred to the MRO spacecraft flight computer for processing (e.g., data compression) before transmission to Earth. The ground data system and operations are based on 9 years of Mars Global Surveyor Mars Orbiter Camera on-orbit experience. CTX has been allocated 12% of the total MRO data return, or about ≥3 terabits for the nominal mission. This data volume would cover ∼9% of Mars at 6 m/pixel, but overlapping images (for stereo, mosaics, and observation of changes and meteorological events) will reduce this area. CTX acquired its first (instrument checkout) images of Mars on 24 March 2006.

https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2006JE002808

Context Camera Investigation on board the Mars Reconnaissance Orbiter

Singer, F. Nimmo, W. B. McKinnon, J. M. Moore, K. Ennico, C. B. Olkin, P. Schenk, J. R. Spencer, S. A. Stern, H. A. Weaver, L. A. Young, and the New Horizons Team. Sagan Center at the SETI Institute, NASA Ames Research Center, Southwest Research Institute, Boulder, University of California, Santa Cruz, Washington University in St. Louis, Lunar and Planetary Institute, Johns Hopkins University Applied Physics Laboratory.

Landslides in the Serenity Chasma Region, Charon

Mao, J.M. Moore, J.R. Spencer, F. Nimmo, L.A. Young, C.B. Olkin, K. Ennico, H.A. Weaver, S.A. Stern, and the New Horizons Geology, Geophysics & Imaging Theme Team; Dept. Earth and Planet. Sci. & McDonnell Center for the Space Sci., Washington Univ. in St. Louis, Saint Louis, MO 63130 (mckinnon@wustl.edu), LPI, Houston, TX 77058, NASA Ames Research Center, Moffett Field, CA 94035, SwRI, Boulder, CO 80302, Dept. Earth and Planetary Sci., UC Santa Cruz, Santa Cruz CA, 95064, JHUAPL, Laurel, MD 20723.

Impact Origin of Sputnik Planitia Basin, Pluto

An impact basin origin for sputnik “planitia” and surrounding terrains, pluto

HABITABILITY. R. T. Pappalardo, D. A. Senske, H. Korth, D. Blaney, D. Blankenship, P. Christensen, S. Kempf, C. Raymond, K. Retherford, E. P. Turtle, J. H. Waite, J. Westlake, G. C. Collins, K. Hand, J. Lunine, M. McGrath, F. Nimmo, C. Paty, J. Soderblom, J. R. Spencer, C. Paranicas, S. Solomon, and the Europa Science Team. Jet Propulsion Laboratory, California Inst. Technology, Pasadena, CA, Johns Hopkins Univ. Applied Physics Laboratory, Laurel, MD, UTIG, Austin, TX, SESE, Ariz. State Univ., Tempe, AZ, LASP, Univ. Colorado, Boulder, CO, SWRI, San Antonio, TX, Wheaton College, Norton, MA, CAPS, Cornell Univ., Ithaca, NY, SETI Inst., Mountain View, CA, UCSC, Santa Cruz, CA, EAS, Georgia Tech., Atlanta, GA, EAPS, MIT, Cambridge, MA, SWRI, Boulder, CO, Lamont-Doherty Earth Observatory, Palisades, NY.

The Europa Multiple-Flyby Mission: Synergistic Science to Investigate Habitability

/pdf/geophysical-controls-on-martian-post-impact-hydrothermal-405noy3mso.pdf

Geophysical Controls on Martian Post-Impact Hydrothermal Systems

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