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

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BOX 5.2 The Discovery Program’s Value to Exploring the Inner Planets The Discovery program continues to be an essential part of the exploration and scientific study of the inner planets. Their proximity to Earth and the Sun enable easy access by spacecraft in the Discovery class. During the past decade inner planets science has benefited greatly from the Discovery program. Past and ongoing missions include: • MESSENGER—The first mission to orbit Mercury; and • GRAIL—An effort to use high-quality gravity field mapping of the moon to determine the moon’s interior structure (scheduled for launch in 2011). In addition, recent and planned missions to the Moon, although not Discovery missions, are generally equivalent to other missions in that program. The orbital LRO and impactor LCROSSE missions address both exploration and science goals for characterizing the lunar surface and identifying potential resources, while LADEE will characterize the lunar atmosphere and dust environment. The proximity and ready accessibility of the inner planets provides opportunities to benefit from the frequent launch schedule envisioned by this program. Although Discovery missions are competitively and not strategically selected, Mercury, Venus and the Moon offer many science opportunities for Discovery teams to seek to address. The most recent Discovery announcement of opportunity attracted over two dozen proposals, including a number of inner planets proposals. At Mercury, orbital missions that build on the results from MESSENGER could characterize high-latitude, radar-reflective volatile deposits, map the chemistry and mineralogy of the surface, measure the composition of the atmosphere, characterize the stability and morphology of the magnetosphere, and precisely determine the long-term planetary rotational state. At Venus, platforms including orbiters, balloons, and probes could be used to study atmospheric chemistry and dynamics, surface geochemistry and topography, and current and past surface and interior processes. The proximity of the Moon makes it an ideal target for future orbital or landed Discovery missions, building on the rich scientific findings of recent lunar missions, and the planned GRAIL and LADDE missions. The variety of tectonic, volcanic and impact structures, as well as chemical and mineralogical diversity offer significant opportunity for future missions. REFERENCES 1. The term inner planets is used here to refer to Mercury, Venus and the Moon. Whereas, the term terrestrial planets is used to refer to Earth, Mercury, Venus, Mars, and the Moon. 2. Although scientific and programmatic issues relating to Mars are described in Chapter 6, it is not always possible to entirely divorce martian studies from studies of the other terrestrial planets. Therefore, when issues concerning Mercury, Venus, or the Moon naturally touch upon corresponding issues relevant to Mars they are mentioned in the spirit of comparative planetology. 3. R. Jeanloz, D.L. Mitchell, A.L. Sprague, and I de Pater. 1995. Evidence for a basalt-free surface on Mercury and implications for internal heat. Science 268(5216):1455-1457, doi: 10.1126/science.7770770. D.T. Blewett, M.S. Robinson, B.W. Denevi, J.J. Gillis-Davis, J.W. Head, S.C. Solomon, G.M. Holsclaw, and W.E. McClintock. 2009. Multispectral images of Mercury from the first MESSENGER flyby: Analysis of global and regional color trends. Earth Planet. Sci. Lett. 285:272-282, doi: 10.1016/j.epsl.2009.02.021. PREPUBLICATION COPY—SUBJECT TO FURTHER EDITORIAL CORRECTION 5-25
4. D.J. Lawrence, W.C. Feldman, J.O. Goldsten, T.J. McCoy, D.T. Blewett, W.V. Boynton, L.G. Evans, L.R. Nittler, E.G. Rhodes, and S.C. Solomon. 2010. Identification and measurement of neutronabsorbing elements on Mercury’s surface, Icarus, in press, doi: 10.1016/j.icarus.2010.04.005. 5. J.L. Margot, S.J. Peale, R.F. Jurgens, M.A. Slade, and I.V. Holin. 2007. Large longitude libration of Mercury reveals a molten core. Science 316(5825):710-714, doi: 10.1126/science.1140514. D.E. Smith, M.T. Zuber, R.J. Phillips, S.C. Solomon, G.A. Neumann, F.G. Lemoin, S.J. Peale, J.- L. Margot, M.H. Torrence, M.J. Talpe, J.W. Head III, S.A. Hauck II, C.L. Johnson, M.E. Perry, O.S. Barnouin, R.L. McNutt, Jr., and J. Oberst. 2010. The equatorial shape and gravity field of Mercury from MESSENGER flybys 1 and 2. Icarus, in press, doi:10.1016/j.icarus.2010.04.007. 6. B.J. Anderson, M.H.. Acuña, H. Korth, M.E. Purucker, C.L. Johnson, J.A. Slavin, S.C. Solomon, and R.L. McNutt, Jr. 2008. The structure of Mercury’s magnetic field from MESSENGER’s first flyby. Science 321(5885):82-85, doi: 10.1126/science.1159081. 7. B.W. Denevi, M.S. Robinson, S.C. Solomon, S.L. Murchie, D.T. Blewett, D.L. Domingue, T.J. McCoy, C.M. Ernst, J.W. Head, T.R. Watters, and N.L. Chabot 2009. The evolution of Mercury’s crust: A global perspective from MESSENGER. Science 324(5927):613-618. J.W. Head, C.M. Weitz, and L. Wilson. 2002. Dark ring in southwestern Orientale Basin: Origin as a single pyroclastic eruption. J. Geophys. Res. 107:E1, doi: 10.1029/2000JE001438. 8. N. Mueller, J. Helbert, G.L. Hashimoto, C.C.C. Tsang, S. Erard, G. Piccioni, and P. Drossart. 2008. Venus surface thermal emission at 1 μm in VIRTIS imaging observations: Evidence for variation of crust and mantle differentiation conditions. Journal of Geophysical Research 113:E00B17, doi:10.1029/2008JE003225. G.L. Hashimoto, M. Roos-Serote, S. Sugita, M.S. Gilmore, L.W. Kamp, R.W. Carlson, and K.H. Baines. 2008. Felsic highland crust on Venus suggested by Galileo Near-Infrared Mapping Spectrometer data. J. Geophys. Res. 113:E00B24, doi:10.1029/2008JE003134. 9. S.E. Smrekar, E.R. Stofan, N. Mueller, A. Treiman, L. Elkins-Tanton, J. Helbert, G. Piccioni, and P. Drossart. 2010. Recent hotspot volcanism on Venus from VIRTIS emissivity data. Science 328(5978):605-608, doi:10.1126/science.1186785. 10. T.R. Watters, S.C. Solomon, M.S. Robinson, J.W. Head, S.L. André, S.A. Hauck II, and S.L. Murchie. 2009. The tectonics of Mercury: The view after MESSENGER’s first flyby. Earth Planet. Sci. Lett. 285(3-4):283-296. B.W. Denevi, M.S. Robinson, S.C. Solomon, S.L. Murchie, D.T. Blewett, D.L. Domingue, T.J. McCoy, C.M. Ernst, J.W. Head, T.R. Watters, and N.L. Chabot. 2009. The evolution of Mercury’s crust: A global perspective from MESSENGER. Science 324(5927):613-618. J.W. Head, S.L. Murchie, L.M. Prockter, S.C. Solomon, C.R. Chapman, R.G. Strom, T.R. Watters, D.T. Blewett, J.J. Gillis-Davis, C.I. Fassett, J.L. Dickson, G.A. Morgan, and L. Kerber. 2009. Volcanism on Mercury: Evidence from the first MESSENGER flyby for extrusive and explosive activity and the volcanic origin of plains. Earth Planet. Sci. Letters 285: 227-242. 11. See, for example, K. Tsiganis, R. Gomes, A. Morbidelli, and H.F. Levison. 2005. Origin of the orbital architecture of the giant planets of the solar system. Nature 435:459-461, doi: 10.1038/nature03539. 12. S.E. Smrekar, E.R. Stofan, N. Mueller, A. Treiman, L. Elkins-Tanton, J. Helbert, G. Piccioni, and P. Drossart. 2010. Recent hotspot volcanism on Venus from VIRTIS emissivity data. Science 328(5978):605-608, doi:10.1126/science.1186785. 13. N. Mueller, J. Helbert, G.L. Hashimoto, C.C.C. Tsang, S. Erard, G. Piccioni, and P. Drossart. 2008. Venus surface thermal emission at 1 μm in VIRTIS imaging observations: Evidence for variation of crust and mantle differentiation conditions. Journal of Geophysical Research 113:E00B17, doi: 10.1029/2008JE003225. PREPUBLICATION COPY—SUBJECT TO FURTHER EDITORIAL CORRECTION 5-26
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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.
Page 101 and 102: 4 The Primitive Bodies: Building Bl
Page 103 and 104: FIGURE 4.1 Asteroids and comet nucl
Page 105 and 106: • How do the compositions of pres
Page 107 and 108: Future Directions for Investigation
Page 109 and 110: Astrobiology is the study of the or
Page 111 and 112: Important Questions Some important
Page 113 and 114: observations of the outer parts of
Page 115 and 116: Sample Curation and Laboratory Faci
Page 117 and 118: In the previous decadal survey, CCS
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Page 121 and 122: hazard. Asteroid 433 Eros, one of t
Page 123 and 124: BOX 4.1 The Discovery Program, Vita
Page 125 and 126: ody exploration can be achieved by
Page 127 and 128: 34. H.H. Hsieh and D. Jewitt. 2006.
Page 129 and 130: FIGURE 5.1 Mercury, Venus, and the
Page 131 and 132: Constrain the Bulk Composition of t
Page 133 and 134: from Venus Express and Galileo may
Page 135 and 136: • Understand the composition and
Page 137 and 138: • Is there evidence of environmen
Page 139 and 140: Important Questions Some important
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Page 143 and 144: that may have fostered life, there
Page 145 and 146: • Venus In Situ Explorer • Sout
Page 147 and 148: FIGURE 5.3 Venus’s climate is con
Page 149 and 150: Important scientific objectives tha
Page 151: BOX 5.1 Planetary Roadmaps Roadmaps
Page 155 and 156: 6 Mars: Evolution of an Earth-like
Page 157 and 158: BOX 6.1 Mars Science Laboratory Sch
Page 159 and 160: live there now?”—both key compo
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Page 165 and 166: UNDERSTAND THE PROCESSES AND HISTOR
Page 167 and 168: FIGURE 6.4 Examples of recent clima
Page 169 and 170: particularly the polar-layered depo
Page 171 and 172: FIGURE 6.6 Geologic time sequence o
Page 173 and 174: Future Directions for Investigation
Page 175 and 176: planets and for understanding subse
Page 177 and 178: experiments, compounded by the unce
Page 179 and 180: Curation Martian samples require sc
Page 181 and 182: particle sizes, wavelength ranges,
Page 183 and 184: environmental conditions including
Page 185 and 186: Mars Polar Climate Mission As a fol
Page 187 and 188: R.E. Arvidson, C.C. Allen, D.J. Des
Page 189 and 190: 27. J. Grotzinger, J.F. Bell III, W
Page 191 and 192: B.M. Jakosky and R.J. Phillips. 200
Page 193 and 194: 72. White papers received by decada
Page 195 and 196: (MRR-SAG). Posted by the Mars Explo
Page 197 and 198: the solar system formed. Understand
Page 199 and 200: FIGURE 7.2 Left: This Hubble image
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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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54. White papers received by decada
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92. White papers received by decada
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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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Future Directions for Investigation
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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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Future Directions for Investigation
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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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particular technology item. In gene
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The Requirement for Power Of all th
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proposals and populated by technolo
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TABLE 11.1 Summary of Types of Miss
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Solar System Access and Other Core
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influence on the planetary science
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A Letter of Request and Statement o
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latter topics are treated in the NR
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main findings and recommendations s
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TABLE B.1 Institutional Distributio
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M. Gudipati, Laboratory Studies for
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Scott A. Sandford, The Comet Coma R
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C Cost and Technical Evaluation of
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were all full mission studies selec
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Schedule To aid in the assessment o
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FIGURE C.3 Complexity Based Risk As
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Lunar Lander Network⎯Four Landers
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Caching Mars Rover Mars Astrobiolog
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Mars Sample Return Lander and Mars
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Flagship‐class Europa Orbiter SOU
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Saturn Atmospheric Entry Probe SOUR
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Enceladus Orbiter Spacecraft SOURCE
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Uranus Orbiter with Entry Probe SOU
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SUMMARY Linked technical, cost, and
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Overview The purpose of this rapid
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Conclusions Based on analyses of th
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Technology development was found to
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• Characterize the local meteorol
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• Characterize Ganymede’s uniqu
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landing in the small southern lakes
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atmospheric probe and another a sep
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FIGURE E.1 Projected budget for the
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Biosphere: The life zone of Earth o
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EPOXI: The name of the extended mis
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Late heavy bombardment: A postulate
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Nili Fossae region: A fracture in t
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Protoplanet: A planet in the proces
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Stardust: A spacecraft launched in
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G Mission and Technology Study Repo
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