1.1 Core

Earth's core, a crucial component of our planet's structure, plays a vital role in geochemistry and global processes. Its composition, primarily iron and nickel with lighter elements, influences heat distribution and generates Earth's magnetic field through complex convection patterns.

The core's extreme conditions challenge direct observation, requiring innovative research approaches. Understanding its formation, evolution, and current state is essential for interpreting geophysical data and modeling Earth's past and future, including the geodynamo and planetary magnetic field.

Structure of Earth's core

• Earth's core plays a crucial role in geochemistry by influencing global heat distribution and generating the planet's magnetic field
• Understanding core structure provides insights into Earth's formation, evolution, and current geodynamic processes
• Core composition and properties significantly impact mantle dynamics and surface geological phenomena

Composition of inner core

Top images from around the web for Composition of inner core

• 

  Atomic structures of twin boundaries in hexagonal close-packed metallic crystals with particular ... View original

  Is this image relevant?

• 

  Deformation twinning mechanism in hexagonal-close-packed crystals | Scientific Reports View original

  Is this image relevant?

• 

  Frontiers | The BCC-FCC Phase Transformation Pathways and Crystal Orientation Relationships in ... View original

  Is this image relevant?

• 

  Atomic structures of twin boundaries in hexagonal close-packed metallic crystals with particular ... View original

  Is this image relevant?

• 

  Deformation twinning mechanism in hexagonal-close-packed crystals | Scientific Reports View original

  Is this image relevant?

1 of 3

Top images from around the web for Composition of inner core

• 

  Atomic structures of twin boundaries in hexagonal close-packed metallic crystals with particular ... View original

  Is this image relevant?

• 

  Deformation twinning mechanism in hexagonal-close-packed crystals | Scientific Reports View original

  Is this image relevant?

• 

  Frontiers | The BCC-FCC Phase Transformation Pathways and Crystal Orientation Relationships in ... View original

  Is this image relevant?

• 

  Atomic structures of twin boundaries in hexagonal close-packed metallic crystals with particular ... View original

  Is this image relevant?

• 

  Deformation twinning mechanism in hexagonal-close-packed crystals | Scientific Reports View original

  Is this image relevant?

1 of 3

• Primarily composed of solid iron-nickel alloy with ~5% nickel
• Contains small amounts of light elements (sulfur, oxygen, silicon) to account for density deficit
• Exhibits a hexagonal close-packed crystal structure under extreme pressure
• Anisotropic properties suggest preferential crystal alignment or flow patterns

Composition of outer core

• Consists of liquid iron-nickel alloy with ~10% lighter elements
• Light element candidates include sulfur, oxygen, carbon, hydrogen, and silicon
• Composition inferred from seismic velocities and density constraints
• Convection in outer core drives geodynamo and planetary magnetic field

Core-mantle boundary

• Marks the transition between silicate mantle and metallic core at ~2900 km depth
• Characterized by large contrasts in density, viscosity, and chemical composition
• Exhibits complex topography with variations up to 5-10 km
• Hosts D" layer, a region of anomalous seismic properties and potential chemical interactions

Physical properties

• Core physical properties determine Earth's internal dynamics and energy budget
• Extreme conditions in the core challenge direct measurements and require innovative research approaches
• Understanding core properties is essential for interpreting geophysical observations and modeling Earth's evolution

Temperature of the core

• Outer core temperature ranges from ~4000-5000 K at core-mantle boundary
• Inner core temperature estimated at ~5000-6000 K
• Temperature gradient drives convection and heat flow from core to mantle
• Melting point depression by light elements affects inner core crystallization

Pressure in the core

• Pressure increases with depth due to overlying rock and metal layers
• Core-mantle boundary pressure ~136 GPa
• Center of Earth pressure reaches ~364 GPa
• High pressure alters material properties and phase relationships

Density vs depth

• Density increases with depth due to compression and compositional changes
• Outer core density ranges from ~9.9-12.2 g/cm³
• Inner core density ~12.8-13.1 g/cm³
• Density jump at inner core boundary ~0.5-0.8 g/cm³ due to solidification

Core formation

• Core formation processes shaped Earth's early geochemical differentiation
• Understanding these processes helps explain current elemental distributions in Earth's layers
• Core formation theories inform models of planetary accretion and evolution

Accretion and differentiation

• Earth formed through collision and merger of planetesimals and planetary embryos
• High-energy impacts caused widespread melting and metal-silicate separation
• Gravitational segregation led to sinking of dense metallic material to form the core
• Timescale of core formation estimated at ~30-100 million years after solar system formation

Siderophile element partitioning

• Siderophile (iron-loving) elements preferentially partition into metallic core
• Includes platinum group elements (Pt, Pd, Ir) and moderately siderophile elements (Ni, Co)
• Partitioning behavior depends on pressure, temperature, and oxygen fugacity
• Observed mantle abundances used to constrain core formation conditions

Core growth over time

• Initial rapid core formation followed by slower continuous growth
• Late veneer addition after main core formation added some siderophiles to mantle
• Crystallization of inner core began ~1-1.5 billion years ago
• Ongoing light element segregation may contribute to core evolution

Geodynamo and magnetic field

• Earth's magnetic field is generated by convection in the liquid outer core
• The geodynamo process is fundamental to understanding Earth's deep interior and surface environment
• Magnetic field variations provide insights into core dynamics and planetary evolution

Convection in outer core

• Driven by compositional and thermal buoyancy forces
• Coriolis effect due to Earth's rotation organizes flow into columnar structures
• Convection patterns influenced by inner core growth and mantle heat flux variations
• Typical flow velocities estimated at ~10^-4 to 10^-3 m/s

Magnetic field generation

• Convection of electrically conductive fluid creates self-sustaining dynamo
• Toroidal and poloidal field components interact to maintain field
• Field strength at core-mantle boundary ~0.1-1 mT
• Polarity reversals occur irregularly on geological timescales

Paleomagnetic record

• Magnetic minerals in rocks preserve Earth's ancient field directions
• Provides evidence for plate tectonic motions and continental reconstructions
• Records geomagnetic polarity reversals and excursions
• Used to study long-term core dynamics and inner core growth history

Geochemical tracers

• Geochemical tracers provide indirect information about core composition and processes
• Analyzing trace element and isotopic signatures helps constrain core formation conditions
• Integrating geochemical data with geophysical observations improves core models

Isotopic signatures

• W-Hf isotope system constrains timing of core formation
• Fe isotopes may indicate core-mantle interaction or inner core crystallization
• Nd, Pb isotopes in mantle plumes suggest possible core contribution
• Noble gas isotopes (He, Ne) provide insights into early Earth differentiation

Siderophile element abundances

• Highly siderophile elements (HSEs) in mantle indicate late veneer addition
• Moderately siderophile elements constrain pressure-temperature conditions of core formation
• Refractory siderophile elements (Mo, W) sensitive to oxidation state during accretion
• Volatile siderophile elements (Pb, Ag) inform models of volatile depletion during planet formation

Light element partitioning

• Si partitioning between metal and silicate affected by pressure and oxygen fugacity
• O partitioning influenced by temperature and FeO content of mantle
• S behavior depends on pressure and degree of metal-silicate equilibration
• H potentially incorporated through reaction with hydrous minerals during accretion

Core-mantle interaction

• Core-mantle boundary (CMB) is a critical interface for heat and chemical exchange
• Processes at CMB influence both mantle dynamics and core evolution
• Understanding core-mantle interactions is crucial for interpreting seismic observations and geochemical signatures

Chemical exchange at boundary

• Potential for iron from core to react with mantle minerals (ferropericlase, bridgmanite)
• Light elements may diffuse from core into lowermost mantle
• Possibility of core-derived noble gases in mantle plumes
• Partial melting at CMB could facilitate element transfer

Thermal boundary layer

• Thin layer (~100-300 km) above CMB with large temperature gradient
• Controls heat flow from core to mantle
• Influences convection patterns in both core and mantle
• May contain partial melt or chemically distinct materials

Plume generation

• Thermal instabilities in boundary layer can initiate mantle plumes
• Large low shear velocity provinces (LLSVPs) may act as plume sources
• Core heat contribution affects plume buoyancy and ascent rates
• Geochemical signatures in plume-derived lavas may reflect core influence

Seismic observations

• Seismic waves provide primary means of probing Earth's deep interior
• Core structure and properties inferred from travel times and wave characteristics
• Seismic data essential for constraining composition and dynamics of the core

P-wave vs S-wave behavior

• P-waves (compressional) travel through both liquid and solid core
• S-waves (shear) cannot propagate through liquid outer core, creating shadow zone
• P-wave velocity decreases and S-wave velocity drops to zero at core-mantle boundary
• PKP waves refracted through core used to study core structure

Velocity structure

• P-wave velocity in outer core ranges from ~8-10 km/s
• Inner core P-wave velocity ~11 km/s
• Velocity discontinuity at inner core boundary due to solidification
• Velocity gradients provide information on composition and thermal state

Anisotropy in inner core

• Seismic waves travel faster along Earth's rotation axis than in equatorial plane
• Suggests preferential alignment of iron crystals or flow patterns
• Degree of anisotropy varies with depth and between eastern and western hemispheres
• May reflect inner core growth processes or past deformation history

Core cooling and evolution

• Core cooling drives Earth's thermal and magnetic evolution
• Understanding cooling rate and mechanisms crucial for predicting future geodynamo behavior
• Core thermal history linked to mantle dynamics and surface geological processes

Heat flow from core

• Total heat flow across core-mantle boundary estimated at 5-15 TW
• Contributions from secular cooling, latent heat of inner core crystallization, and gravitational energy release
• Heat flow pattern may be heterogeneous due to mantle structure
• Cooling rate affects convection vigor and magnetic field generation

Crystallization of inner core

• Began ~1-1.5 billion years ago as core cooled below freezing point
• Releases latent heat and gravitational energy, powering geodynamo
• Crystallization rate estimated at ~0.5-1 mm/year
• Texture and grain size of inner core influenced by cooling rate and deformation

Implications for geodynamo

• Inner core growth stabilizes geodynamo by providing additional energy source
• Changes in cooling rate may affect magnetic field intensity and reversal frequency
• Future scenarios include continued slow cooling or eventual cessation of dynamo
• Thermal evolution models constrained by paleomagnetic data and thermal history of mantle

Planetary comparisons

• Comparing Earth's core to other planetary bodies provides context for understanding core formation and evolution
• Diversity of core structures in solar system informs models of planetary differentiation
• Exoplanet observations expand our understanding of possible core compositions and dynamics

Cores of terrestrial planets

• Mercury: Large core relative to planet size, possibly due to mantle stripping
• Venus: Similar size to Earth, likely has liquid outer core but no global magnetic field
• Mars: Smaller core, partially or fully solidified, extinct global magnetic field
• Moon: Small core (~350 km radius), mostly solidified, weak paleomagnetic field

Gas giant metallic hydrogen cores

• Jupiter and Saturn have massive cores of metallic hydrogen under extreme pressure
• Helium rain-out may occur, affecting core composition and planet evolution
• Strong magnetic fields generated by convection in metallic hydrogen layers
• Core erosion and dissolution into surrounding fluid layers possible

Exoplanet core predictions

• Super-Earths may have diverse core structures depending on formation conditions
• High-pressure phases of iron could exist in cores of massive rocky planets
• Ocean worlds might have cores interacting with deep water layers
• Extreme temperature planets could have exotic core compositions (carbides, silicides)

Experimental techniques

• Studying core conditions requires innovative experimental and computational approaches
• Combining multiple techniques provides complementary constraints on core properties
• Ongoing technological advancements continue to improve our ability to probe extreme core conditions

High-pressure experiments

• Diamond anvil cells compress samples to core pressures (>100 GPa)
• Laser-heated diamond anvil cells achieve simultaneous high pressure and temperature
• Large volume presses (multi-anvil) allow study of larger samples at moderate pressures
• Shock compression experiments probe dynamic behavior at core conditions

Computational modeling

• Ab initio calculations predict material properties at core pressures and temperatures
• Molecular dynamics simulations investigate atomic-scale behavior of core materials
• Geodynamo models simulate core convection and magnetic field generation
• Thermochemical evolution models track core cooling and differentiation over time

Geophysical inversions

• Seismic tomography reveals 3D structure of core-mantle boundary region
• Normal mode oscillations constrain core density and elastic properties
• Magnetic field observations inverted to infer core flow patterns
• Geodetic data (length of day variations, nutations) provide information on core dynamics