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

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Lunar Lander Network⎯Four Landers SOURCE: NASA Mission Study (transmitted from George J. Tahu, NASA Planetary Science Division) Scientific Objectives • Enhance knowledge of lunar interior • Key science themes: – Determine lateral variations in the structure and composition of the lunar crust, upper mantle, lower mantle, and lunar core – Determine distribution and origin of lunar seismic activity – Determine the lunar global heat flow budget to better constrain knowledge of lunar thermal evolution – Determine bulk lunar composition of radioactive heat‐ producing elements – Determine nature and origin of lunar crustal magnetic field Key Parameters • Payload – Seismometer – Heat Flow Experiment – Electromagnetic Sounder – Lunar Laser Ranging – Guest Payload – Education/Public Outreach Pancam • Advanced Stirling Radioisotope Generator Surface Power • Launch Mass: 3572 kg (257 kg individual lander mass) • Launch Date: 2016 (on Atlas V 511) • Direct lunar near‐side landing Lunar Geophysical Network Key Challenges • DACS Propulsion – Development needed for MON‐25/MMH combustion stability • Mass – Low dry mass contingency for this development phase – Propulsion requirements multiply impact to overall mass growth • Reliability – Single‐string network reliability • Mission Operations – High tempo operations for multi‐lander cruise and landing phase Key Cost Element Comparison Cost Risk Analysis S‐Curve PREPUBLICATION COPY—SUBJECT TO FURTHER EDITORIAL CORRECTION C-9
Caching Mars Rover SOURCE: NASA Mission Study (transmitted from Lisa May, NASA Planetary Science Division) Scientific Objectives • Perform in situ science on Mars samples to look for evidence of ancient life or pre‐biotic chemistry • Collect, document, and package samples for future collection and return to Earth • Key science themes: – The search for extant life on Mars – The search for evidence of past life on Mars – Understanding martian climate history – Determination of the ages of geologic terrains on Mars – Understanding surface‐atmosphere interactions on Mars – Understanding martian interior processes Key Parameters • Model Payload With Sampling/Caching System – Pancam high resolution stereo imager (on mast) – Near‐Infrared Point Spectrometer – Microscopic Imager – Alpha‐Particle X‐ray Spectrometer – Dual Wavelength Raman/Fluorescence Instrument – Sample Handling, Encapsulation, and Containerization (arm, corer/abrader, organic blank, handling and container system) • Two x 2.2 m diameter Ultraflex solar arrays • Launch Mass: 4457 kg • Launch Date: 2018 (on Atlas V 531) • Orbit: Type I transfer direct to Mars surface – 15° S to 25° N latitude Mars Astrobiology Explorer‐Cacher Key Challenges • Vehicle Capabilities Beyond Mars Science Laboratory – Terrain‐relative descent navigation and precision landing with pallet – Aeroshell volume to accommodate MAX‐C, ExoMars, and pallet – Increased rover traverse speed over MSL and MER • Sample Handling, Encapsulation, and Containerization (SHEC) – Lack of maturity in SHEC subsystem – Affect of planetary protection and sample transfer requirements • Mass – Insufficient mass growth contingency for this development phase – Low launch margin for this development phase Key Cost Element Comparison Cost Risk Analysis S‐Curve PREPUBLICATION COPY—SUBJECT TO FURTHER EDITORIAL CORRECTION C-10
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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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Page 339 and 340: TABLE 11.1 Summary of Types of Miss
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Page 343 and 344: influence on the planetary science
Page 346 and 347: A Letter of Request and Statement o
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Page 350 and 351: main findings and recommendations s
Page 352 and 353: TABLE B.1 Institutional Distributio
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Page 358 and 359: C Cost and Technical Evaluation of
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Page 362 and 363: Schedule To aid in the assessment o
Page 364 and 365: FIGURE C.3 Complexity Based Risk As
Page 368 and 369: Caching Mars Rover Mars Astrobiolog
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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
Page 384 and 385: Conclusions Based on analyses of th
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Page 388 and 389: • Characterize the local meteorol
Page 390 and 391: • Characterize Ganymede’s uniqu
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Page 396 and 397: FIGURE E.1 Projected budget for the
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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