Note: Cover -- Half-title -- Series information -- Title page -- Copyright information -- Table of contents -- List of Contributors -- 1 Planetesimals -- Acknowledgments -- References -- Part One Dynamical Evolution -- 2 Signatures of Hit-and-run Collisions -- 2.1 Introduction -- 2.1.1 Final Accretion -- 2.2 Catastrophic Disruption -- 2.2.1 Stripping of Mantles -- 2.2.2 Disposal of Rock -- 2.2.3 Orphans and Oligarchs -- 2.3 Surviving Projectiles -- 2.4 Planetesimals to Embryos -- 2.4.1 Differentiation and Segregation -- 2.4.2 Planetesimals, Embryos, and Shocks -- 2.5 Simulations of Hit and Run -- 2.5.1 Segregation and Clumping -- 2.5.2 Transitions to Giant Impacts -- 2.5.3 Pressure Unloading -- 2.6 Accretion and Attrition -- 2.6.1 Hiding in Plain Sight -- 2.6.2 Hit-and-run Return -- 2.7 Conclusions -- Acknowledgments -- References -- 3 Using the Main Asteroid Belt to Constrain Planetesimal and Planet Formation -- 3.1 Introduction -- 3.2 Constraints for Collisional Evolution -- 3.2.1 Wavy Main Belt Size Frequency Distribution -- 3.2.2 Asteroid Families -- 3.2.3 Impact Basins on Vesta -- 3.2.4 Near-Earth Asteroids and Lunar Craters -- 3.2.5 Additional Constraints -- 3.3 Reconstructing the Original Asteroid Belt -- 3.3.1 A Brief Description of Generic Collisional Models -- 3.3.2 Estimating Collisional Evolution in the Primordial Main Belt -- 3.4 Formation and Dynamical Constraints for the Main Belt Asteroids -- 3.4.1 Could the Asteroid Belt Have Formed With Low Mass? -- 3.4.2 Orbital Excitation, Radial Mixing -- 3.5 Modeling Work Compared with Constraints -- 3.5.1 Formation of the Present-day Asteroid Belt from a Low-mass Belt -- 3.5.2 Formation of the Present-day Asteroid Belt from a Massive Mass Belt -- I. Migration of Planetary Embryos -- II. Stirring from a Population of Resident Embryos -- III. Migration of Jupiter Through the Asteroid Belt. , 3.6 Conclusions -- Acknowledgments -- References -- Part Two Chemical and Mineralogical Diversity -- 4 Differentiation Under Highly Reducing Conditions: New Insights from Enstatite Meteorites and Mercury -- 4.1 Introduction -- 4.2 Insights from Aubrites -- 4.3 Implications for Mercury -- 4.4 Summary -- References -- 5 Origin and Evolution of Volatile-rich Asteroids -- 5.1 Introduction -- 5.2 C-Type Asteroid Inventory -- 5.3 Origin Scenarios and Accretional Environments -- 5.3.1 Accretion Timeframe -- 5.3.2 Original Composition -- 5.3.3 Accretion Timescale -- 5.4 Processes Driving the Evolution of Volatile-rich Bodies -- 5.4.1 Aqueous Alteration -- 5.4.2 Salt Production -- 5.4.3 Hydrothermal Circulation -- 5.4.4 Physical Differentiation -- 5.5 Differentiation of Large Volatile-rich Asteroids -- 5.6 Addressing Differentiation at Ceres with the Dawn Mission -- 5.7 Summary -- Acknowledgments -- References -- 6 Silicate Melting and Volatile Loss During Differentiation in Planetesimals -- 6.1 Introduction -- 6.2 Radiogenic Heating and Volatile Contents of Early Planetesimals -- 6.3 The Fate of Volatiles -- 6.4 The Fate of Silicate Melts -- 6.5 Implications -- 6.6 Summary -- Acknowledgments -- References -- 7 Iron and Stony-iron Meteorites: Evidence for the Formation, Crystallization, and Early Impact Histories of Differentiated Planetesimals -- 7.1 Introduction -- 7.2 Taxonomy and Associations -- 7.3 Fractionally Crystallized Iron Meteorites -- 7.4 Silicate-bearing Iron Meteorites -- 7.5 Mesosiderites and Pallasites -- 7.5.1 Melting and Differentiation of the Pallasite and Mesosiderite Parent Bodies -- 7.5.2 Origin of Pallasite and Mesosiderite Breccias -- 7.6 Summary -- Acknowledgments -- References -- 8 Arguments for the Non-existence of Magma Oceans in Asteroids -- 8.1 Introduction: The Ambiguity of the Term ''Magma Ocean'' Applied to Asteroids. , 8.2 Physical Issues -- 8.2.1 Heat Source and Heating Prior to Melting -- 8.2.2 The Onset of Melting -- 8.2.3 Melt Migration -- 8.2.4 Melt Accumulation -- 8.3 Geochemical and Petrological Issues -- 8.3.1 Meteorite Evidence Relevant to the Magma Ocean Concept for Asteroids -- 8.3.2 Meteorite Evidence for the Degree of Fe,Ni-FeS and Silicate Melting on Asteroids -- Compositional Information Summary -- 8.4 Summary -- Acknowledgments -- References -- 9 Magnetic Fields on Asteroids and Planetesimals -- 9.1 Introduction -- 9.2 Meteoritic Paleomagnetism -- 9.2.1 Magnetic Fields Recorded in Meteorites -- 9.2.2 Magnetic Fields in Asteroids -- 9.3 Core Formation -- 9.4 Planetesimal Dynamos -- 9.4.1 Modeling Methods -- 9.4.2 Planetesimal Dynamo Models -- 9.5 Core Crystallization -- 9.5.1 Physics of Core Crystallization -- 9.5.2 Dynamos During Core Crystallization -- 9.6 Alternative Magnetization Mechanisms -- 9.6.1 Dynamo Alternatives to Core Convection -- 9.6.2 The Solar Nebula Magnetic Environment -- 9.7 Summary -- Acknowledgments -- References -- 10 Magnetic Mineralogy of Meteoritic Metal: Paleomagnetic Evidence for Dynamo Activity on Differentiated Planetesimals -- 10.1 Introduction -- 10.2 Mineral Magnetism of Meteoritic Metal -- 10.2.1 Summary of Microstructural Changes in Zoned Taenite -- 10.2.2 X-ray Photo-emission Electron Microscopy -- 10.2.3 Magnetic Microstructures of Zoned Taenite -- 10.3 Dynamo Activity on the Main-group Pallasite Parent Body -- 10.3.1 Paleomagnetic Constraints on Origin of the Main-group Pallasites -- 10.3.2 Nanopaleomagnetic Constraints on the Properties of the Pallasite Core Dynamo -- 10.4 Opportunities for Future Studies -- 10.5 Summary -- Acknowledgments -- References -- 11 Chronology of Planetesimal Differentiation -- 11.1 Introduction -- 11.2 Dating Methods -- 11.2.1 Extinct and Extant Chronometers. , 11.2.2 Model Ages for Dating Differentiation -- 11.3 Chronology of Core Formation -- 11.3.1 Iron Meteorites -- 11.3.2 Angrites and Eucrites -- 11.3.3 Distinct Stages of Melt Segregation During Core Formation -- 11.3.4 Link Between Differentiation and Accretion Timescales -- 11.4 Timescales of Silicate Differentiation and Crust Formation -- 11.4.1 Silicate Differentiation -- 11.4.2 Crust Formation -- 11.5 Conclusions -- Acknowledgments -- References -- 12 Stable Isotope Evidence for the Differentiation and Evolution of Planetesimals -- 12.1 Introduction -- 12.2 Iron Isotopic Constraints on Temperature and Composition -- 12.2.1 Chondritic Reference Frame -- 12.2.2 Pallasites - a natural analog for differentiation -- 12.2.3 Mars - Compositional Variations -- 12.2.4 Vesta -- 12.2.5 Aubrites -- 12.2.6 Angrites -- 12.3 Silicon Isotopic Constraints on Composition and Oxygen Fugacity -- 12.3.1 Chondritic Reference Frame -- 12.3.2 Mars -- 12.3.3 Vesta -- 12.3.5 Aubrites -- 12.3.6 Angrites -- 12.4 Zinc Isotopic Constraints on Volatility -- 12.4.1 Chondritic Reference Frame -- 12.4.2 Tektites -- 12.4.3 Differentiated Meteorites -- 12.4.4 The Moon -- 12.5 Summary -- Acknowledgments -- References -- Part Three Asteroids as Records of Formation and Differentiation -- 13 Composition of Solar System Small Bodies -- 13.1 Introduction -- 13.2 Main-belt Asteroids -- 13.2.1 S-Complex Asteroids -- Surface Composition -- Bulk Composition -- 13.2.2 C-Complex Asteroids -- Surface Composition -- Bulk Composition -- 13.2.3 P- and D-Type Asteroids -- Surface Composition -- Bulk Composition -- 13.2.4 Remaining Asteroid (A-, K-, L-, M-, O-, R-, V-, Xe-, Xc-, and Xk-) Types -- Surface Composition -- Bulk Composition -- 13.3 Jupiter Trojans -- 13.3.1 Surface composition -- 13.3.2 Bulk Composition -- 13.4 Irregular Satellites of the Giant Planets -- 13.4.1 Surface Composition. , 13.4.2 Bulk Composition -- 13.5 Neptune Trojans -- 13.5.1 Surface Composition -- 13.5.2 Bulk Composition -- 13.6 KBOs -- 13.6.1 Surface Composition -- 13.6.2 Bulk Composition -- 13.7 Comets -- 13.7.1 Volatiles -- 13.7.2 Dust -- 13.7.3 Bulk Composition -- 13.8 Decoding the Solar System's Past -- 13.8.1 Constraints on Current Dynamical Models (Grand Tack, Nice Model) -- 13.8.2 Primordial Architecture -- Spatial Distribution -- Temporal Distribution -- 13.9 Conclusions -- Acknowledgments -- References -- 14 Evidence for Differentiation among Asteroid Families -- 14.1 Introduction -- 14.2 Vesta Family -- 14.3 Flora Family -- 14.4 Eunomia Family -- 14.5 Eos Family -- 14.6 Hungaria Family -- 14.7 Merxia and Agnia Families -- 14.8 Absence of A-types among Asteroid Families -- 14.9 Absence of a Ceres Family -- 14.10 Conclusions -- Acknowledgments -- References -- 15 Dawn at Vesta: Paradigms and Paradoxes -- 15.1 Introduction -- 15.2 Vesta as a Differentiated Protoplanet -- 15.2.1 Evidence from HEDs -- 15.2.2 Evidence from Density Distribution and Core Size -- 15.3 The Case of the Missing Olivine -- 15.3.1 Olivine on Vesta's Surface -- 15.3.2 Olivine Distribution at Depth -- 15.4 Architecture of Vesta's Crust and Mantle -- 15.4.1 The Crust-Mantle Conundrum -- 15.4.2 Crustal Structure and Igneous Processes -- 15.5 Water on Vesta -- 15.6 Implications for Formation and Evolution of Planetesimals -- 15.7 Summary -- Acknowledgments -- References -- 16 Planetesimals in Debris Disks -- 16.1 Introduction -- 16.2 The Formation of Planetesimals -- 16.3 Planetesimals and Planetary Debris Disks -- 16.4 Dust Production and Evolution in Debris Disks -- 16.4.1 Collisional Timescales -- 16.4.2 Collisional Cascades -- 16.4.3 Non-gravitational Forces on Small Particles -- 16.5 Planetesimals and Debris: Common Patterns -- 16.5.1 Very Hot Dust. , 16.5.2 Hot Dust in the Terrestrial Planet Zone.

Note: Förderkennzeichen BMWi 01MG13001G. - Verbund-Nummer 01142925 , Paralleltitel dem englischen Berichtsblatt entnommen , Literaturverzeichnis: Blatt 40-42 , Unterschiede zwischen dem gedruckten Dokument und der elektronischen Ressource können nicht ausgeschlossen werden , Mit deutscher und englischer Zusammenfassung

Note: Auch als gedr. Ausg. vorhanden , Zugl.: Karlsruhe, KIT, Diss., 2010 , Systemvoraussetzungen: Acrobat reader.