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  • 1
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    Architecting the Communication and Navigation Networks for NASA's Space Exploration Systems (2007)
    In:  CASI
    Details
    Publication Date: 2019-07-13
    Description: NASA is planning a series of short and long duration human and robotic missions to explore the Moon and then Mars. A key objective of the missions is to grow, through a series of launches, a system of systems communication, navigation, and timing infrastructure at minimum cost while providing a network-centric infrastructure that maximizes the exploration capabilities and science return. There is a strong need to use architecting processes in the mission pre-formulation stage to describe the systems, interfaces, and interoperability needed to implement multiple space communication systems that are deployed over time, yet support interoperability with each deployment phase and with 20 years of legacy systems. In this paper we present a process for defining the architecture of the communications, navigation, and networks needed to support future space explorers with the best adaptable and evolable network-centric space exploration infrastructure. The process steps presented are: 1) Architecture decomposition, 2) Defining mission systems and their interfaces, 3) Developing the communication, navigation, networking architecture, and 4) Integrating systems, operational and technical views and viewpoints. We demonstrate the process through the architecture development of the communication network for upcoming NASA space exploration missions.
    Keywords: Lunar and Planetary Science and Exploration
    Type: E-16232 , International Conference on System of Systems Engineering (SoSE); Apr 16, 2007 - Apr 18, 2007; San Antonio, TX; United States
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  • 2
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    Properties of Rubble-Pile Asteroid (101955) Bennu from OSIRIS-REx Imaging and Thermal Analysis (2019)
    In:  CASI
    Details
    Publication Date: 2019-08-14
    Description: Establishing the abundance and physical properties of regolith and boulders on asteroids is crucial for understanding the formation and degradation mechanisms at work on their surfaces. Using images and thermal data from NASA's Origins, Spectral Interpretation, Resource Identification, and Security-Regolith Explorer (OSIRIS-REx) spacecraft, we show that asteroid (101955) Bennu's surface is globally rough, dense with boulders, and low in albedo. The number of boulders is surprising given Bennu's moderate thermal inertia, suggesting that simple models linking thermal inertia to particle size do not adequately capture the complexity relating these properties. At the same time, we find evidence for a wide range of particle sizes with distinct albedo characteristics. Our findings imply that ages of Bennu's surface particles span from the disruption of the asteroid's parent body (boulders) to recent in situ production (micrometre-scale particles).
    Keywords: Lunar and Planetary Science and Exploration
    Type: GSFC-E-DAA-TN67770 , Nature Astronomy (e-ISSN 2397-3366); 3; 341–351
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  • 3
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    Jupiter's atmospheric composition from the Cassini thermal infrared spectroscopy experiment (2004)
    In:  Other Sources
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    Publication Date: 2011-08-24
    Description: The Composite Infrared Spectrometer observed Jupiter in the thermal infrared during the swing-by of the Cassini spacecraft. Results include the detection of two new stratospheric species, the methyl radical and diacetylene, gaseous species present in the north and south auroral infrared hot spots; determination of the variations with latitude of acetylene and ethane, the latter a tracer of atmospheric motion; observations of unexpected spatial distributions of carbon dioxide and hydrogen cyanide, both considered to be products of comet Shoemaker-Levy 9 impacts; characterization of the morphology of the auroral infrared hot spot acetylene emission; and a new evaluation of the energetics of the northern auroral infrared hot spot.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Science (ISSN 0036-8075); Volume 305; 5690; 1582-6
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  • 4
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    Imaging Jupiter's aurorae from H3+ emissions in the 3-4 micrometers band (1991)
    In:  Other Sources
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    Publication Date: 2011-08-24
    Description: Since H3+ was first spectroscopically detected on Jupiter, there has been considerable interest in using this simple molecular ion to probe conditions existing in the planet's auroral regions. Here we present a series of images of Jupiter recorded at wavelengths sensitive to emission by H3+, which reveal the spatial distribution of excited H3+ molecular ions in the jovian ionosphere, as seen from Earth. We believe that they provide high-spatial-resolution images of polar aurorae on Jupiter. They suggest that the intensity of the auroral emission can vary on a timescale of an hour, a shorter period than had previously been noted. We also find that the spatial distribution of H3+ emissions correlates only partially with the loci of auroral activity inferred from ultraviolet and longer-wavelength infrared observations. The H3+ emission may therefore be controlled by auroral processes that are different from those responsible for the ultraviolet and infrared emissions.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Nature (ISSN 0028-0836); Volume 353; 539-42
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  • 5
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    Mars Stratigraphy Mission (2000)
    In:  CASI
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    Publication Date: 2004-12-03
    Description: The Mars Stratigraphy Mission lands a rover on the surface of Mars which descends down a cliff in Valles Marineris to study the stratigraphy. The rover carries a unique complement of instruments to analyze and age-date materials encountered during descent past 2 km of strata. The science objective for the Mars Stratigraphy Mission is to identify the geologic history of the layered deposits in the Valles Marineris region of Mars. This includes constraining the time interval for formation of these deposits by measuring the ages of various layers and determining the origin of the deposits (volcanic or sedimentary) by measuring their composition and imaging their morphology.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Concepts and Approaches for Mars Exploration; Part 1; 50-51; LPI-Contrib-1062
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  • 6
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    Atmospheric Science and the JIMO Mission (2003)
    In:  CASI
    Details
    Publication Date: 2004-10-30
    Description: The Jupiter Icy Moons Orbiter mission will intensely study Callisto, Ganymede and Eu- ropa for several years. During its orbital tour, there will be long periods (approximately 300 days) where the spacecraft is spiraling in from one satellite to the next, giving the perfect opportunity to study Jupiter's atmosphere. The obvious question is, 'Why do we need JIMO to do this, after Voyager, Galileo and the Cassini flyby?' Much like the satellite science from these missions, atmospheric science still has many outstanding questions, some of which were raised by these missions. In addition, virtually every measurable quantity on Jupiter varies both spatially and temporally, and previous missions did not supply the coverage needed to address them. The JIMO mission offers an outstanding opportunity for the global and long temporal coverage needed to answer these questions.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Forum on Concepts and Approaches for Jupiter Icy Moons Orbiter; 75; LPI-Contrib-1163
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  • 7
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    Artificial Crater Formation on Satellite Surfaces Using an Orbiting Railgun (2003)
    In:  CASI
    Details
    Publication Date: 2004-10-30
    Description: The specification of greater than 45kW of disposable power available on the JIMO spacecraft raises the possibility of a new class of instrumentation that has utility at such power levels. In this presentation we discuss the concept of an electromagnetic mass driver that can launch projectiles from orbit around one of the Galilean satellites directed on a trajectory that will impact the satellite surface. The resulting impact will create a crater that will provide information on the mechanical properties of surface and near-surface materials, expose subsurface materials for remote spectral identification, and form a vapor cloud that can be sensed for composition either remotely or in-situ. An analog for such a controlled cratering experiment is Deep Impact, a mission to observe the crater and ensuing ejecta cloud formed by a ballistic projectile into a comet surface in July, 2005.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Forum on Concepts and Approaches for Jupiter Icy Moons Orbiter; 18; LPI-Contrib-1163
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  • 8
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    Temperatures, winds, and composition in the saturnian system (2005)
    In:  Other Sources
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    Publication Date: 2011-08-24
    Description: Stratospheric temperatures on Saturn imply a strong decay of the equatorial winds with altitude. If the decrease in winds reported from recent Hubble Space Telescope images is not a temporal change, then the features tracked must have been at least 130 kilometers higher than in earlier studies. Saturn's south polar stratosphere is warmer than predicted from simple radiative models. The C/H ratio on Saturn is seven times solar, twice Jupiter's. Saturn's ring temperatures have radial variations down to the smallest scale resolved (100 kilometers). Diurnal surface temperature variations on Phoebe suggest a more porous regolith than on the jovian satellites.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Science (ISSN 0036-8075); Volume 307; 5713; 1247-51
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  • 9
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    Mars Exploration Architecture (2000)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: The architecture of NASA's program of robotic Mars exploration missions received an intense scrutiny during the summer months of 1998. We present here the results of that scrutiny, and describe a list of Mars exploration missions which are now being proposed by the nation's space agency. The heart of the new program architecture consists of missions which will return samples of Martian rocks and soil back to Earth for analysis. A primary scientific goal for these missions is to understand Mars as a possible abode of past or present life. The current level of sophistication for detecting markers of biological processes and fossil or extant life forms is much higher in Earth-based laboratories than possible with remotely deployed instrumentation, and will remain so for at least the next decade. Hence, bringing Martian samples back to Earth is considered the best way to search for the desired evidence. A Mars sample return mission takes approximately three years to complete. Transit from Earth to Mars requires almost a single year. After a lapse of time of almost a year at Mars, during which orbital and surface operations can take place, and the correct return launch energy constraints are met, a Mars-to-Earth return flight can be initiated. This return leg also takes approximately one year. Opportunities to launch these 3-year sample return missions occur about every 2 years. The figure depicts schedules for flights to and from Mars for Earth launches in 2003, 2005, 2007 and 2009. Transits for less than 180 deg flight angle, measured from the sun, and more than 180 deg are both shown.
    Keywords: Lunar and Planetary Science and Exploration
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  • 10
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    An Assessment of the Issues and Concerns Associated with the Analysis of Ice-bearing Samples by the 2009 Mars Science Laboratory (2003)
    In:  CASI
    Details
    Publication Date: 2017-10-02
    Description: In early 2003, the Mars Icy Sample Team (MIST) was formed to address several questions related to the acquisition and analysis of ice-bearing samples on the surface of Mars by a robotic mission. These questions were specifically framed in the context of planning for the 2009 Mars Science Laboratory (MSL) lander, but the answers will also also have value in planning other future landed investigations.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Third International Conference on Mars Polar Science and Exploration; LPI-Contrib-1184
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