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

More documents

Recommendations

Info

decades ago. NASA rightly takes responsibility for the curation and distribution of planetary materials. Collections of extraterrestrial materials are composed of: • Samples that are delivered naturally to Earth in the form of meteorites and interplanetary dust particles, and • Samples collected by spacecraft missions and returned to Earth for study. Recent sample return missions include Genesis, which collected samples of the solar wind, and Stardust, which collected cometary material as it flew through the coma of Comet Wild 2. These missions continue a legacy of sample return that includes the robotic Luna and the human Apollo missions to the Moon. Currently, two sample return missions are under Phase-A study for NASA’s New Frontiers program: OSIRIS-REx as a sample return mission to Near-Earth Asteroid 1999 RQ36, and MoonRise as a sample return mission to the South Pole-Aitken Basin region of the Moon. The missions recommended in Chapter 9 also include return of samples from a comet nucleus and Mars. In the next decade, then, requirements for sample curation will rapidly grow to become of highest priority. Samples to be returned to Earth from many planetary bodies (e.g., the Moon, asteroids, and comets) are given a planetary protection designation of “Unrestricted Earth Return” as they are not regarded as posing any biohazard to Earth. However, future sample return missions from Mars and other targets that might potentially harbor life (e.g. Europa and Enceladus) are classified as “Restricted Earth Return” and are subject to quarantine restrictions, requiring special receiving and curation facilities that can preserve the pristine nature of the returned materials and prevent potential contamination of Earth. Such a Sample Receiving Facility (SRF) has been discussed in detail for Mars Sample Return, 14,15,16 and would also need to be considered for return from other targets that are classified as Restricted Earth Return. Consistent with past recommendations in the reports cited above, a SRF for Restricted Earth Return samples would provide the following: • Biohazard assessment (following established protocols for life detection); • Sterilization of samples for potential early release; and • Release from containment of samples deemed to be safe, and transfer to appropriate curation facilities. Current biohazard facilities focus predominantly on sample containment and so existing biocontainment facilities would not be optimal for receiving and characterizing the hazards associated with extraterrestrial materials. Nonetheless, it is a good policy, where appropriate, to use existing capabilities to reduce cost and risk, while maintaining the required safety requirements. A coordinated approach to all potentially hazardous returned samples is needed that leverages the considerable expertise within NASA and the scientific community in working with extraterrestrial samples. As plans move forward for Restricted Earth Return missions, including Mars sample return, NASA should establish a single advisory group to provide input on all aspects of collection, containment, characterization and hazard assessment, and allocation of such samples. This advisory group must have an international component. The major site for curation and distribution of extraterrestrial samples within the United States is the Astromaterials Acquisition and Curation Office (AACO) of the Astromaterials Research and Exploration Science division at NASA’s Johnson Space Center. The AACO oversees the preparation and allocation of samples for research and education, initial characterization of new samples, and secure preservation for the benefit of future generations. Sample allocation decisions are performed under the guidance of the Curation and Analysis Planning Team for Extraterrestrial Materials (CAPTEM) and the Meteorite Working Group (MWG), both supported through the Lunar PREPUBLICATION COPY—SUBJECT TO FURTHER EDITORIAL CORRECTION 10-16
and Planetary Institute. Currently, the JSC’s AACO has separate laboratories that support curation and distribution of Apollo lunar samples, Antarctic meteorites, Stardust cometary materials, Genesis solar wind samples, cosmic dust collected in upper atmosphere flights, and space-exposed hardware. Plans are in place for a new asteroid laboratory if OSIRIS-REx is selected as the next New Frontiers mission, and for expansion of the lunar laboratory if MoonRise is selected. Sample curation facilities are critical components of any sample return mission, and must be designed specifically for the types of returned materials and handling requirements. Early planning and adequate funding are needed early in the mission cycle so that an adequate facility is available once samples are returned and deemed ready for curation and distribution. Particular challenges for the future include cryogenic handling of materials from comets, asteroids, the icy satellites, and the frigid depths of unlit craters on the Moon and Mercury, as well as biocontainment of samples from Mars and other targets of biological interest. Every sample return mission flown by NASA should explicitly include in the estimate of its cost to the agency the full costs required for appropriate initial sample curation. The cost estimates for sample return missions recommended in Chapter 9 of this report include these curation costs. The most important instruments for any sample return mission are the ones in the laboratories on Earth. To derive the full scientific return from sample return missions, it is critical to maintain technical and instrumental capabilities for initial sample characterization, as well as foster expansion to encompass appropriate new analytical instrumentation as it becomes available and as different sample types are acquired. It is equally crucial for NASA to maintain technical and instrumental capability in the sample science community. The development of new laboratory instrumentation is just as important for sample return missions as is development of new spacecraft instruments for other planetary missions. Well before planetary missions return samples, NASA should establish a well-coordinated and integrated program for development of the next generation of laboratory instruments to be used in sample characterization and analysis. SUPPORTING RESEARCH AND RELATED ACTIVITIES AT NSF The National Science Foundation’s principal support for planetary science is provided by the Division of Astronomical Sciences in the Directorate for Mathematical and Physical Sciences. The Astronomy and Astrophysics Research Grants (AAG) Program, for example, provides individual investigator and collaborative research grants for observational, theoretical, laboratory, and archival data studies in all areas of astronomy and astrophysics, including planetary astronomy. Planetary astronomy themes include planetary interiors, surfaces, and atmospheres, planetary satellites, comets and asteroids, trans-Neptune objects, the interplanetary medium, and the origin and evolution of the solar system. Typical awards are in the range $95,000 to $125,000 per year for a nominal 3-year period. The focus of the program is scientific merit with broad impact and the potential for transformative research. Planetary scientists can also be supported directly through various career programs. In short, NSF supports nearly all areas of planetary science except space missions, which it supports indirectly through laboratory research and archived data. Further contributions to planetary science are realized through investigator grants in the Directorate for Geosciences, and by NSF support of major observatory facilities that are open to planetary scientists, Antarctic meteorite collection and curation, and the study of Antarctic geomorphic analogs to ancient Mars. NSF grants and support for field activities are a very important source of support for a limited subset of planetary science activities in the U.S., and should continue. PREPUBLICATION COPY—SUBJECT TO FURTHER EDITORIAL CORRECTION 10-17
Page 1 and 2:
PREPUBLICATION COPY Subject to Furt
Page 3 and 4:
The National Academy of Sciences is
Page 5 and 6:
COMMITTEE ON THE PLANETARY SCIENCE
Page 7 and 8:
STAFF DAVID H. SMITH, Senior Progra
Page 9 and 10:
Preface Strategic planning activiti
Page 11 and 12:
statement of task’s call for “i
Page 13 and 14:
Understand the Processes That Contr
Page 15 and 16:
Executive Summary In recent years,
Page 17 and 18:
however, that the Discovery program
Page 19 and 20:
• Jupiter Europa Orbiter (descope
Page 21 and 22:
TABLE ES.2 Medium Class Missions—
Page 23 and 24:
Summary This report was requested b
Page 25 and 26:
• Recent volcanic activity on Ven
Page 27 and 28:
Mission Study Process and Technical
Page 29 and 30:
Near the end of the past decade, NA
Page 31 and 32:
• Mars Astrobiology Explorer-Cach
Page 33 and 34:
development, and descoped or cancel
Page 35 and 36:
Plausible circumstances could impro
Page 37 and 38:
Data Distribution and Archiving Dat
Page 39 and 40:
Sample curation facilities are crit
Page 41 and 42:
consider making equivalent systems
Page 43 and 44:
committee concluded that for the mo
Page 45 and 46:
alanced ground-based solar astronom
Page 47 and 48:
1 Introduction to Planetary Science
Page 49 and 50:
THE 2002 SOLAR SYSTEM EXPLORATION D
Page 51 and 52:
Medium The first decadal survey ide
Page 53 and 54:
FIGURE 1.6 Victoria crater as image
Page 55 and 56:
FIGURE 1.8 The mirror for the Large
Page 57 and 58:
FIGURE 1.10 From a comet, to the de
Page 59 and 60:
• The committee’s programmatic
Page 61 and 62:
• Opportunities for joint venture
Page 63 and 64:
FIGURE 1.14 Schematic showing the f
Page 65 and 66:
2 National and International Progra
Page 67 and 68:
FIGURE 2.3 Sand dunes on Mars photo
Page 69 and 70:
NASA’s Earth Science Division Pla
Page 71 and 72:
More recently, among the goals of t
Page 73 and 74:
FIGURE 2.6 A natural bridge on the
Page 75 and 76:
investigations should still be deve
Page 77 and 78:
FIGURE 2.10 The surface of Titan as
Page 79 and 80:
3 Shared objectives that incorporat
Page 81 and 82:
3 Priority Questions in Planetary S
Page 83 and 84:
• How have the myriad chemical an
Page 85 and 86:
How Did the Giant Planets and Their
Page 87 and 88:
heavy bombardment? Clues to address
Page 89 and 90:
Did Mars or Venus Host Ancient Aque
Page 91 and 92:
We lack critical geophysical data a
Page 93 and 94:
detected in time. The report conclu
Page 95 and 96:
How Have the Myriad of Chemical and
Page 97 and 98:
13. P.R. Estrada, I. Mosqueira, J.J
Page 99 and 100:
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
Page 119 and 120:
asteroid (either ice-rock or metal-
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
Page 141 and 142:
timescales, including the possible
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 and 152:
BOX 5.1 Planetary Roadmaps Roadmaps
Page 153 and 154:
4. D.J. Lawrence, W.C. Feldman, J.O
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
Page 161 and 162:
characteristics (water, gradients i
Page 163 and 164:
availability, physicochemical facto
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:
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
Page 201 and 202:
temperatures, helium is enhanced in
Page 203 and 204:
FIGURE 7.4 The intrinsic specific l
Page 205 and 206:
Investigate the Chemistry of Giant
Page 207 and 208:
Jupiters seen around other stars in
Page 209 and 210:
• What causes the enormous differ
Page 211 and 212:
FIGURE 7.5 Top: This composite comp
Page 213 and 214:
EXPLORING THE GIANT PLANET’S ROLE
Page 215 and 216:
destroy areas of land equivalent to
Page 217 and 218:
• Assess tidal evolution within g
Page 219 and 220:
• What processes drive the visibl
Page 221 and 222:
esolution visible and near-infrared
Page 223 and 224:
INTERCONNECTIONS Links to Other Par
Page 225 and 226:
SUPPORTING RESEARCH AND RELATED ACT
Page 227 and 228:
FIGURE 7.10 Our atmosphere blocks l
Page 229 and 230:
Cassini Solstice Mission ADVANCING
Page 231 and 232:
8. Determine the composition, struc
Page 233 and 234:
Summary To achieve the primary goal
Page 235 and 236:
Outer Solar System; William B. McKi
Page 237 and 238:
Page 239 and 240:
Page 241 and 242:
TABLE 8.1 Characteristics of the La
Page 243 and 244:
organisms live there now?” Titan
Page 245 and 246:
• Why are Titan and Callisto appa
Page 247 and 248:
Callisto but unlike Ganymede. This
Page 249 and 250:
valuable window into solar system h
Page 251 and 252:
Page 253 and 254:
FIGURE 8.6 Multiple jets, dominated
Page 255 and 256:
FIGURE 8.8 Schematic of the complex
Page 257 and 258:
orbits of Io and Europa), and poten
Page 259 and 260:
Cassini has revealed that most of t
Page 261 and 262:
satellite interiors should include
Page 263 and 264:
Page 265 and 266:
hardened technology for Io and Gany
Page 267 and 268:
FIGURE 8.11 After a comprehensive t
Page 269 and 270:
FIGURE 8.12 Galileo color image of
Page 271 and 272:
Titan Saturn System Mission Many Ti
Page 273 and 274: 1. What is the nature of Enceladus
Page 275 and 276: the majority of the Jupiter Europa
Page 277 and 278: 7. O. Mousis, J.I. Lunine, M. Pasek
Page 279 and 280: 45. K.K. Khurana, M.G. Kivelson, K.
Page 281 and 282: 9 Recommended Flight Investigations
Page 283 and 284: All of the recommendations below ar
Page 285 and 286: As discussed in more detail below,
Page 287 and 288: • Ensure that there are adequate
Page 289 and 290: TABLE 9.2 Discovery Program Mission
Page 291 and 292: overarching questions in Chapter 3.
Page 293 and 294: These five were selected from the s
Page 295 and 296: The Mars community, in their inputs
Page 297 and 298: should immediately undertake an eff
Page 299 and 300: (a) (b) FIGURE 9.1 Notional funding
Page 301 and 302: As noted, the recommended and cost-
Page 303 and 304: described above are the existing De
Page 305 and 306: The projected need decreased from 2
Page 307 and 308: partnership with the Department of
Page 309 and 310: 10 Planetary Science Research and I
Page 311 and 312: Through the direct involvement of s
Page 313 and 314: Theoretical development and numeric
Page 315 and 316: Defining the Need Jon Miller, in hi
Page 317 and 318: efforts, can help assure compatibil
Page 319 and 320: history. And telescopic observation
Page 321 and 322: Hubble Space Telescope Hubble obser
Page 323: Although Ka-band downlink has a cle
Page 327 and 328: the Green Bank Telescope (GBT), and
Page 329 and 330: up observations. Likewise, monitori
Page 331 and 332: 11 The Role of Technology Developme
Page 333 and 334: particular technology item. In gene
Page 335 and 336: The Requirement for Power Of all th
Page 337 and 338: proposals and populated by technolo
Page 339 and 340: TABLE 11.1 Summary of Types of Miss
Page 341 and 342: Solar System Access and Other Core
Page 343 and 344: influence on the planetary science
Page 346 and 347: A Letter of Request and Statement o
Page 348 and 349: latter topics are treated in the NR
Page 350 and 351: main findings and recommendations s
Page 352 and 353: TABLE B.1 Institutional Distributio
Page 354 and 355: M. Gudipati, Laboratory Studies for
Page 356 and 357: Scott A. Sandford, The Comet Coma R
Page 358 and 359: C Cost and Technical Evaluation of
Page 360 and 361: were all full mission studies selec
Page 362 and 363: Schedule To aid in the assessment o
Page 364 and 365: FIGURE C.3 Complexity Based Risk As
Page 366 and 367: Lunar Lander Network⎯Four Landers
Page 368 and 369: Caching Mars Rover Mars Astrobiolog
Page 370 and 371: Mars Sample Return Lander and Mars
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
Page 386 and 387:
Technology development was found to
Page 388 and 389:
• Characterize the local meteorol
Page 390 and 391:
• Characterize Ganymede’s uniqu
Page 392 and 393:
landing in the small southern lakes
Page 394 and 395:
atmospheric probe and another a sep
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
show all

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

Create successful ePaper yourself

Delete template?

Save as template?