Vision and Voyages for Planetary Science in the - Solar System ...

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Conclusions Based on analyses of the mechanical, thermal, power, avionics, and communication designs for the probe and the carrier spacecraft, a Venus mission using the metallic bellows architecture for shortlived (~5 hrs) aerial mobility is technically feasible. The cost estimate for the nominal baseline mission was estimated to be in the flagship range. The cost is driven by the metallic bellows and supporting mechanisms for its operation. Technology development, accommodation, and complex integration also contribute to the high cost of the probe. VENUS INTREPID TESSERA LANDER A mission concept study performed by NASA’s Goddard Space Flight Center and NASA’s Ames Research Center. Overview The purpose of this enhanced rapid mission architecture study was to investigate a mission capable of safely landing in one of the mountainous tessera regions of Venus. This mission concept provides key measurements of surface chemistry and mineralogy and imaging of a tessera region, as well as new measurements of important atmospheric species that can answer fundamental questions about the evolution of Venus. Science Objectives • Characterize chemistry and mineralogy of the Venus surface. • Place constraints on the size and temporal extent of a possible ocean in Venus’s past. • Characterize the morphology and relative stratigraphy of surface units. Mission Design The mission design elements include a carrier spacecraft to be used as a communications relay and a two-element probe. The probe elements are: the Venus lander; and the entry and descent element including aeroshell and parachute systems. The lander’s design focuses on enabling a safe landing in the rough tessera terrain. The launch opportunity considered was for 2021, with fly-by and descent/landing mission elements in 2022. Mission Challenges The most significant challenges posed by this mission were related to the development of a high- TRL level Raman/laser-induced breakdown spectroscopy (LIBS) system, safe landing, and testing at Venus environmental conditions. To reduce risk, advancements in two key technology areas are needed: first, verifying the Raman/LIBS implementation, calibrated operation, and sizing for the Venus surface environment, including high entry loads on the laser and second, additional analyses and testing to ensure safe landing in potentially rugged terrains (at lander scales). PREPUBLICATION COPY—SUBJECT TO FURTHER EDITORIAL CORRECTION D-4
Conclusions Venus’ tessera provide fundamental clues to the planet’s past, but, the terrain has been viewed as largely inaccessible for landed science due to their known roughness. Based on analyses of the landing dynamics, mechanical, thermal, power, optics, avionics, and communication designs for this mission, a robust spacecraft capable of landing safely in the tessera terrain, conducting surface science and transmitting all data back to Earth via the telecom-relay spacecraft is technically feasible. However, because the Venus In Situ Explorer and Venus Climate Mission were judged of higher priority combined with considerations of program balance, this mission was not considered further as a decadal option. LUNAR POLAR VOLATILES EXPLORER A mission concept study performed by NASA’s Marshall Space Flight Center in cooperation with the Johns Hopkins University Applied Physics Laboratory. Overview The purpose of this rapid mission architecture study was to determine the feasibility of a mission to investigate putative volatiles in permanently shadowed areas of the lunar poles. While previous orbital missions have provided data that support the possibility of water ice deposits existing in the polar region, this concept seeks to understand the nature of those volatiles by direct in-situ measurement. Science Objectives • Determine the form and species of the volatile compounds at the lunar poles. • Determine the vertical distribution and concentration of volatile compounds in the lunar polar regolith. • Determine the lateral distribution/concentration of volatile compounds in the lunar polar regolith. • Determine the secondary alteration mineralogy of regolith. • Determine the composition and variation in the lunar exosphere adjacent to cold traps. Mission Design The mission concept explored involves placing a lander and instrumented rover in a permanently shadowed crater near one of the Moon’s poles. The rover would carry a suite of science instruments to investigate the location, composition, and state of volatiles. Rovers powered by batteries and radioisotope power systems (RPS) were considered. A battery-powered option, designed to support 4.4 days of surface operations, could achieve some, but not all, the mission’s top science goals. The development of the mission was assumed to start in 2013 to support an October 2018 launch. Mission Challenges Although this study identifies several mission components at TRLs less than 6, the required technology advancements are believed to be achievable and consistent with the outlined mission schedule. PREPUBLICATION COPY—SUBJECT TO FURTHER EDITORIAL CORRECTION D-5
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PREPUBLICATION COPY Subject to Furt
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The National Academy of Sciences is
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COMMITTEE ON THE PLANETARY SCIENCE
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STAFF DAVID H. SMITH, Senior Progra
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Preface Strategic planning activiti
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statement of task’s call for “i
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Understand the Processes That Contr
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Executive Summary In recent years,
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however, that the Discovery program
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• Jupiter Europa Orbiter (descope
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TABLE ES.2 Medium Class Missions—
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Summary This report was requested b
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• Recent volcanic activity on Ven
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Mission Study Process and Technical
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Near the end of the past decade, NA
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• Mars Astrobiology Explorer-Cach
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development, and descoped or cancel
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Plausible circumstances could impro
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Data Distribution and Archiving Dat
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Sample curation facilities are crit
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consider making equivalent systems
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committee concluded that for the mo
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alanced ground-based solar astronom
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1 Introduction to Planetary Science
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THE 2002 SOLAR SYSTEM EXPLORATION D
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Medium The first decadal survey ide
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FIGURE 1.6 Victoria crater as image
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FIGURE 1.8 The mirror for the Large
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FIGURE 1.10 From a comet, to the de
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• The committee’s programmatic
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• Opportunities for joint venture
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FIGURE 1.14 Schematic showing the f
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2 National and International Progra
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FIGURE 2.3 Sand dunes on Mars photo
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NASA’s Earth Science Division Pla
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More recently, among the goals of t
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FIGURE 2.6 A natural bridge on the
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investigations should still be deve
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FIGURE 2.10 The surface of Titan as
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3 Shared objectives that incorporat
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3 Priority Questions in Planetary S
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• How have the myriad chemical an
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How Did the Giant Planets and Their
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heavy bombardment? Clues to address
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Did Mars or Venus Host Ancient Aque
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We lack critical geophysical data a
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detected in time. The report conclu
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How Have the Myriad of Chemical and
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13. P.R. Estrada, I. Mosqueira, J.J
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51. M.J. Mumma, G.L. Villanueva, R.
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4 The Primitive Bodies: Building Bl
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FIGURE 4.1 Asteroids and comet nucl
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• How do the compositions of pres
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Future Directions for Investigation
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Astrobiology is the study of the or
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Important Questions Some important
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observations of the outer parts of
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Sample Curation and Laboratory Faci
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In the previous decadal survey, CCS
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asteroid (either ice-rock or metal-
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hazard. Asteroid 433 Eros, one of t
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BOX 4.1 The Discovery Program, Vita
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ody exploration can be achieved by
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34. H.H. Hsieh and D. Jewitt. 2006.
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FIGURE 5.1 Mercury, Venus, and the
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Constrain the Bulk Composition of t
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from Venus Express and Galileo may
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• Understand the composition and
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• Is there evidence of environmen
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Important Questions Some important
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timescales, including the possible
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that may have fostered life, there
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• Venus In Situ Explorer • Sout
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FIGURE 5.3 Venus’s climate is con
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Important scientific objectives tha
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BOX 5.1 Planetary Roadmaps Roadmaps
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4. D.J. Lawrence, W.C. Feldman, J.O
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6 Mars: Evolution of an Earth-like
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BOX 6.1 Mars Science Laboratory Sch
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live there now?”—both key compo
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characteristics (water, gradients i
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availability, physicochemical facto
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UNDERSTAND THE PROCESSES AND HISTOR
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FIGURE 6.4 Examples of recent clima
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particularly the polar-layered depo
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FIGURE 6.6 Geologic time sequence o
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planets and for understanding subse
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experiments, compounded by the unce
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Curation Martian samples require sc
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particle sizes, wavelength ranges,
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environmental conditions including
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Mars Polar Climate Mission As a fol
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R.E. Arvidson, C.C. Allen, D.J. Des
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27. J. Grotzinger, J.F. Bell III, W
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B.M. Jakosky and R.J. Phillips. 200
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72. White papers received by decada
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(MRR-SAG). Posted by the Mars Explo
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the solar system formed. Understand
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FIGURE 7.2 Left: This Hubble image
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temperatures, helium is enhanced in
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FIGURE 7.4 The intrinsic specific l
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Investigate the Chemistry of Giant
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Jupiters seen around other stars in
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• What causes the enormous differ
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FIGURE 7.5 Top: This composite comp
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EXPLORING THE GIANT PLANET’S ROLE
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destroy areas of land equivalent to
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• Assess tidal evolution within g
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• What processes drive the visibl
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esolution visible and near-infrared
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INTERCONNECTIONS Links to Other Par
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SUPPORTING RESEARCH AND RELATED ACT
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FIGURE 7.10 Our atmosphere blocks l
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Cassini Solstice Mission ADVANCING
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8. Determine the composition, struc
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Summary To achieve the primary goal
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Outer Solar System; William B. McKi
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TABLE 8.1 Characteristics of the La
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organisms live there now?” Titan
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• Why are Titan and Callisto appa
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Callisto but unlike Ganymede. This
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valuable window into solar system h
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FIGURE 8.6 Multiple jets, dominated
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FIGURE 8.8 Schematic of the complex
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orbits of Io and Europa), and poten
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Cassini has revealed that most of t
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satellite interiors should include
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hardened technology for Io and Gany
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FIGURE 8.11 After a comprehensive t
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FIGURE 8.12 Galileo color image of
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Titan Saturn System Mission Many Ti
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1. What is the nature of Enceladus
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the majority of the Jupiter Europa
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7. O. Mousis, J.I. Lunine, M. Pasek
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45. K.K. Khurana, M.G. Kivelson, K.
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9 Recommended Flight Investigations
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All of the recommendations below ar
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As discussed in more detail below,
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• Ensure that there are adequate
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TABLE 9.2 Discovery Program Mission
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overarching questions in Chapter 3.
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These five were selected from the s
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The Mars community, in their inputs
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should immediately undertake an eff
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(a) (b) FIGURE 9.1 Notional funding
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As noted, the recommended and cost-
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described above are the existing De
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The projected need decreased from 2
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partnership with the Department of
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10 Planetary Science Research and I
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Through the direct involvement of s
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Theoretical development and numeric
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Defining the Need Jon Miller, in hi
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efforts, can help assure compatibil
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history. And telescopic observation
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Hubble Space Telescope Hubble obser
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Although Ka-band downlink has a cle
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and Planetary Institute. Currently,
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the Green Bank Telescope (GBT), and
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up observations. Likewise, monitori
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11 The Role of Technology Developme
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Page 372 and 373: Flagship‐class Europa Orbiter SOU
Page 374 and 375: Saturn Atmospheric Entry Probe SOUR
Page 376 and 377: Enceladus Orbiter Spacecraft SOURCE
Page 378 and 379: Uranus Orbiter with Entry Probe SOU
Page 380 and 381: SUMMARY Linked technical, cost, and
Page 382 and 383: Overview The purpose of this rapid
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Page 398 and 399: Biosphere: The life zone of Earth o
Page 400 and 401: EPOXI: The name of the extended mis
Page 402 and 403: Late heavy bombardment: A postulate
Page 404 and 405: Nili Fossae region: A fracture in t
Page 406 and 407: Protoplanet: A planet in the proces
Page 408 and 409: Stardust: A spacecraft launched in
Page 410: G Mission and Technology Study Repo
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