World Library  
Flag as Inappropriate
Email this Article

Planetary core

Article Id: WHEBN0000864017
Reproduction Date:

Title: Planetary core  
Author: World Heritage Encyclopedia
Language: English
Subject: Iron–nickel alloy, InSight, Planetary differentiation, Psyche (spacecraft), Callisto (moon)
Collection: Planetary Geology
Publisher: World Heritage Encyclopedia

Planetary core

Not to be confused with planetary core in the core accretion theory, referring to a central accretionary body surrounded by a halo of dust and gas which serves to trap debris and increase the rate of accretion.
The internal structure of the inner planets.

The planetary core consists of the innermost layer(s) of a planet; which may be composed of solid and liquid layers.[1] Cores of specific planets may be entirely solid or entirely liquid.[2] In our solar system, core size can range from about 20% (Moon) to 85% of a planet's radius (Mercury).

Gas giants also have cores, though the composition of these are still a matter of debate and range in possible composition from traditional stony/iron, to ice or to fluid metallic hydrogen.[3][4][5] Gas giant cores are proportionally much smaller than those of terrestrial planets, though theirs can be considerably larger than the Earth's nevertheless; Jupiter has one 10-30 times heavier than Earth,[5] and exoplanet HD149026 b has a core 67 times the mass of the Earth.[6]


  • Discovery 1
  • Formation 2
    • Accretion 2.1
    • Differentiation 2.2
    • Core merging/impacts 2.3
      • Earth-Moon system 2.3.1
      • Mars 2.3.2
  • Chemistry 3
    • Determining primary composition – Earth 3.1
    • Weight deficit components – Earth 3.2
    • Isotopic composition – Earth 3.3
    • Pallasite meteorites 3.4
  • Dynamics 4
    • Dynamo 4.1
    • Stability and instability 4.2
  • Observed types 5
    • Within the Solar System 5.1
      • Mercury 5.1.1
      • Venus 5.1.2
      • Moon 5.1.3
      • Earth 5.1.4
      • Mars 5.1.5
      • Ganymede 5.1.6
      • Jupiter 5.1.7
      • Saturn 5.1.8
    • Extra-Solar 5.2
      • Chthonian Planets 5.2.1
      • Planets derived from stellar cores and diamond planets 5.2.2
      • Hot ice planets 5.2.3
  • References 6


In 1798, Henry Cavendish calculated the average density of the earth to be 5.48 times the density of water (later refined to 5.53), this led to the accepted belief that the Earth was much denser in its interior.[7] Following the discovery of iron meteorites, Wiechert in 1898 postulated that the Earth had a similar bulk composition to iron meteorites, but the iron had settled to the interior of the Earth, and later represented this by integrating the bulk density of the Earth with the missing iron and nickel as a core.[8] The first detection of Earth's core occurred in 1906 by Richard Dixon Oldham upon discovery of the P-wave shadow zone; the liquid outer core.[9] By 1936 seismologists had determined the size of the overall core as well as the boundary between the fluid outer core and the solid inner core.[10]



Planetary systems form from a flattened disk of dust and gas which accrete rapidly (within thousands of years) into planetesimals around 10 km in diameter. From here gravity takes over to produce Moon to Mars sized planetary embryos (105 - 106 years) and these develop into planetary bodies over an additional 10-100 million years.[11]

Jupiter and Saturn most likely formed around previously existing rocky and/or icey bodies, rendering these previous primordial planets into gas-giant cores.[5] This is the planetary core accretion model of planet formation.


Planetary differentiation is broadly defined as the development from one thing to many things; homogeneous body to several heterogeneous components.[12] The hafnium-182/tungsten-182 isotopic system has a half-life of 9 million years, and is approximated as an extinct system after 45 million years. Hafnium is a lithophile element and tungsten is siderophile element. Thus if metal segregation (between the Earth's core and mantle) occurred in under 45 million years, silicate reservoirs develop positive Hf/W anomalies, and metal reservoirs acquire negative anomalies relative to undifferentiated chondrite material.[11] The observed Hf/W ratios in iron meteorites constrain metal segregation to under 5 million years, the Earth's mantle Hf/W ratio places Earth's core as having segregated within 25 million years.[11] Several factors control segregation of a metal core including the crystallization of perovskite. Crystallization of perovskite in an early magma ocean is an oxidation process and may drive the production and extraction of iron metal from an original silicate melt.

Core merging/impacts

Impacts between planet-sized bodies in the early solar system are important aspects in the formation and growth of planets and planetary cores.

Earth-Moon system

The giant impact hypothesis states that an impact between a theoretical Mars-sized planet Theia and the early Earth formed the modern Earth and moon.[13] During this impact the majority of the iron from Theia and the Earth became incorporated into the Earth's core.[14]


Core merging between the proto-mars and another differentiated planetoid could have been as fast as 1000 years or as slow as 300,000 years (depending on viscosity of both cores).[15]


Determining primary composition – Earth

Using the chondritic reference model and combining known compositions of the crust and mantle, the unknown component, the composition of the inner and outer core, can be determined; 85% Fe, 5% Ni, 0.9% Cr, 0.25% Co, and all other refractory metals at very low concentration.[11] This leaves Earth's core with a 5-10% weight deficit for the outer core[16] and a 4-5% weight deficit for the inner core;[16] which is attributed to lighter elements that should be cosmically abundant and are iron-soluble; H, O, C, S, P, and Si.[11] Earth's core contains half the Earth's vanadium and chromium, and may contain considerable niobium and tantalum.[16] Earth's core is depleted in germanium and gallium.[16]

Weight deficit components – Earth

Sulfur is strongly siderophile and only moderately volatile and depleted in the silicate earth; thus may account for 1.9 weight% of Earth's core.[11] By similar argument; phosphorus may be present up to 0.2 weight%. Hydrogen and carbon, however, are highly volatile and thus would have been lost during early accretion and therefore can only account for 0.1 to 0.2 weight % respectively.[11] Silicon and oxygen thus make up the remaining mass deficit of Earth's core; though the abundances of each are still a matter of controversy revolving largely around the pressure and oxidation state of Earth's core during its formation.[11] No geochemical evidence exists to include any radioactive elements in Earth's core.[16] Despite this, experimental evidence has found potassium to be strongly siderophile given the temperatures associated with core formation, thus there is potential for potassium in planetary cores of planets, and therefore potassium-40 as well.[17]

Isotopic composition – Earth

Hafnium/tungsten (Hf/W) isotopic ratios, when compared with a chondritic reference frame, show a marked enrichment in the silicate earth indicating depletion in Earth's core. Iron meteorites, believed to be resultant from very early core fractionation processes, are also depleted.[11] Niobium/tantalum (Nb/Ta) isotopic ratios, when compared with a chondritic reference frame, show mild depletion in bulk silicate Earth and the moon.[18]

Pallasite meteorites

Pallasites are thought to form at the core-mantle boundary of an early planetesimal, although a recent hypothesis suggests that they are impact-generated mixtures of core and mantle materials.[19]



Dynamo theory is a proposed mechanism to explain how celestial bodies like the Earth generate magnetic fields. The presence or lack of a magnetic field can help constrain the dynamics of a planetary core. Refer to Earth's magnetic field for further details. A dynamo requires a source of thermal and/or compositional buoyancy as a driving force.[18] Thermal buoyancy from a cooling core alone cannot drive the necessary convection as indicated by modelling, thus compositional buoyancy (from changes of phase) is required. On Earth the buoyancy is derived from crystallization of the inner core (which can occur as a result of temperature). Examples of compositional buoyancy include precipitation of iron alloys onto the inner core and liquid immiscibility both which could influence convection both positively and negatively depending on ambient temperatures and pressures associated with the host-body.[18] Other celestial bodies which exhibit magnetic fields are Mercury, Jupiter, Ganymede, and Saturn.[3]

Stability and instability

Small planetary cores may experience catastrophic energy release associated with phase changes within their cores. Ramsey, 1950 found that the total energy released by such a phase change would be on the order of 1029 joules; equivalent to the total energy release due to earthquakes through geologic time. Such an event could explain the asteroid belt. Such phase changes would only occur at specific mass to volume ratios, and an example of such a phase change would be the rapid formation or dissolution of a solid core component.[20]

Observed types

The following summarizes known information about the planetary cores of given non-stellar bodies.

Within the Solar System


Mercury has an observed magnetic field which is believed to be generated within its metallic core.[18] Mercury's core occupies 85% of the planet's radius, making it the largest core relative to the size of the planet in our Solar System; this indicates that much of Mercury's surface may have been lost early in the solar system's history.[21] Mercury has a solid silicate crust and mantle overlying a solid iron sulfide outer core layer, followed by a deeper liquid core layer, and then a possible solid inner core making a third layer.[21]


The composition of Venus' core varies significantly depending on the model used to calculate it, thus constraints are required.[22]

Element Chondritic Model Equilibrium Condensation Model Pyrolitic Model
Iron 88.6% 94.4% 78.7%
Nickel 5.5% 5.6% 6.6%
Cobalt 0.26% Unknown Unknown
Sulfur 5.1% 0% 4.9%
Oxygen 0% Unknown 9.8%


The existence of a lunar core is still debated, however if it does have a core it would have formed synchronously with the Earth's own core at 45 million years post-start of the solar system based on hafnium-tungsten evidence [23] and the giant impact hypothesis. Such a core may have hosted a geomagnetic dynamo early on in its history.[18]


The Earth has an observed magnetic field generated within its metallic core.[18] The Earth has a 5-10% mass deficit for the entire core and a density deficit from 4-5% for the inner core.[16] Fe/Ni value of the core is well constrained by chondritic meteorites.[16] Sulfur, carbon, and phosphorus only account for ~2.5% of the light element component/mass deficit.[16] No geochemical evidence exists for including any radioactive elements in the core.[16] However, experimental evidence has found that potassium is strongly siderophile when dealing with temperatures associated with core-accretion, and thus potassium-40 could have provided an important source of heat contributing to the early Earth's dynamo, though in a lesser extent then on sulfur rich Mars.[17] The core contains half the Earth's vanadium and chromium, and may contain considerable niobium and tantalum.[16] The core is depleted in germanium and gallium.[16] Core mantle differentiation occurred within the first 30 million years of Earth's history.[16] Inner core crystallization timing is still largely unresolved.[16]


Mars possibly hosted a core-generated magnetic field in the past.[18] The dynamo ceased within 0.5 billion years of the planet's formation.[2] Hf/W isotopes derived from the martian meteorite Zagami, indicate rapid accretion and core differentiation of Mars; i.e. under 10 million years.[13] Potassium-40 could have been a major source of heat powering the early martian dynamo.[17]

Core merging between proto-mars and another differentiated planetoid could have been as fast as 1000 years or as slow as 300,000 years (depending on the viscosity of both cores and mantles).[15] Impact-heating of the Martian core would have resulted in stratification of the core and kill the martian dynamo for a duration between 150-200 million years.[15] Modelling done by Williams, et al. 2004 suggests that in order for Mars to have had a functional dynamo, the Martian core was initially hotter by 150 K than the mantle (agreeing with the differentiation history of the planet, as well as the impact hypothesis), and with a liquid core potassium-40 would have had opportunity to partition into the core providing an additional source of heat. The model further concludes that the core of mars is entirely liquid, as the latent heat of crystallization would have driven a longer lasting (greater than one billion years) dynamo.[2] If the core of Mars is liquid, the lower bound for sulfur would be five weight %.[2]


Ganymede has an observed magnetic field generated within its metallic core.[18]


Jupiter has an observed magnetic field generated within its core, indicating some metallic substance is present.[3] Its magnetic field is the strongest in the solar system after the Sun's.

Jupiter has a rock and/or ice core ten-thirty times the mass of the Earth, and this core is likely soluble in the gas envelope above, and so primordial in composition. Since the core still exists, the outer envelope must have originally accreted onto a previously existing planetary core.[5] Thermal contraction/evolution models support the presence of metallic hydrogen within the core in large abundances (greater than Saturn).[3]


Saturn has an observed magnetic field generated within its metallic core.[3] Metallic hydrogen is present within the core (in lower abundances than Jupiter).[3] Saturn has a rock and or ice core ten-thirty times the mass of the Earth, and this core is likely soluble in the gas envelope above, and therefore it is primordial in composition. Since the core still exists, the envelope must have originally accreted onto previously existing planetary cores.[5] Thermal contraction/evolution models support the presence of metallic hydrogen within the core in large abundances (but still less than Jupiter).[3]


Chthonian Planets

A Chthonian planet results when a gas giant has its outer atmosphere stripped away by its parent star, likely due to the planet's inward migration. All that remains from the encounter is the original core.

Planets derived from stellar cores and diamond planets

Carbon planets; previously stars, are formed alongside the formation of a millisecond pulsar. The first such planet discovered was 18 times the density of water, and five times the size of Earth. Thus the planet cannot be gaseous, and must be composed of heavier elements which are also cosmically abundant like carbon and oxygen; making it likely crystalline like a diamond.[24]

PSR J1719-1438 is a 5.7 millisecond pulsar found to have a companion with a mass similar to Jupiter but a density of 23 g/cm3, suggesting that the companion is an ultralow mass carbon white dwarf, likely the core of an ancient star.[25]

Hot ice planets

Exoplanets with moderate densities (more dense than Jovian planets, but less dense than terrestrial planets) suggests that such planets like GJ1214b and GJ436 are composed of primarily water. Internal pressures of such water-worlds would result in exotic phases of water forming on the surface and within their cores.[26]


  1. ^ Solomon, S.C. (2007). "Hot News on Mercury's core". Science 316 (5825): 702–3.   (subscription required)
  2. ^ a b c d Williams, Jean-Pierre; Nimmo, Francis (2004). "Thermal evolution of the Martian core: Implications for an early dynamo". Geology 32 (2): 97–100.  
  3. ^ a b c d e f g Pollack, James B.; Grossman, Allen S.; Moore, Ronald; Graboske, Harold C. Jr. (1977). "A Calculation of Saturn’s Gravitational Contraction History". Icarus (Academic Press, Inc) 30: 111–128.  
  4. ^ Fortney, Jonathan J.; Hubbard, William B. (2003). "Phase separation in giant planets: inhomogeneous evolution of Saturn". Icarus (Academic Press) 164: 228–243.  
  5. ^ a b c d e Stevenson, D. J. (1982). "Formation of the Giant Planets". Planet. Space Sci (Pergamon Press Ltd.) 30 (8): 755–764.  
  6. ^ Sato, Bun'ei; al., et (November 2005). "The N2K Consortium. II. A Transiting Hot Saturn around HD 149026 with a Large Dense Core". The Astrophysical Journal (The American Astronomical Society) 633: 465–473.  
  7. ^ Cavendish, H. (1798). "Experiments to determine the density of Earth". Philosophical Transactions of the Royal Society of London 88: 469–479.  
  8. ^ Wiechert, E. (1897). "Uber die Massenverteilung im Inneren der Erde" [About the mass distribution inside the Earth]. Nachr. K. Ges. Wiss. Goettingen, Math-K.L. (in German): 221–243. 
  9. ^ Oldham, Richard Dixon (1906). "The constitution of the interior of the Earth as revealed by Earthquakes". G.T. Geological Society of London 62: 459–486. 
  10. ^ Transdyne Corporation (2009). J. Marvin Hemdon, ed. "Richard D. Oldham's Discovery of the Earth's Core". Transdyne Corporation. 
  11. ^ a b c d e f g h i Wood, Bernard J.; Walter, Michael J.; Jonathan, Wade (June 2006). "Accretion of the Earth and segregation of its core". Nature Reviews (Nature) 441: 825–833.  
  12. ^ "differentiation". Merriam Webster. 2014. 
  13. ^ a b Halliday; N., Alex (February 2000). "Terrrestrial accretion rates and the origin of the Moon". Earth and Planetary Science Letters (Science) 176 (1): 17–30.  
  14. ^ "A new Model for the Origin of the Moon". SETI Institute. 2012. 
  15. ^ a b c Monteaux, Julien; Arkani-Hamed, Jafar (November 2013). "Consequences of giant impacts in early Mars: Core merging and Martian Dynamo evolution". Journal of Geophysical Research: Planets (AGU Publications): 84–87. 
  16. ^ a b c d e f g h i j k l m McDonough, W. F. (2003). "Compositional Model for the Earth's Core". Geochemistry of the Mantle and Core (Maryland: University of Maryland Geology Department): 547–568. 
  17. ^ a b c Murthy, V. Rama; van Westrenen, Wim; Fei, Yingwei (2003). "Experimental evidence that potassium is a substantial radioactive heat source in planetary cores". letters to nature (Nature) 423: 163–167.  
  18. ^ a b c d e f g h Hauck, S. A.; Van Orman, J. A. (2011). "Core petrology: Implications for the dynamics and evolution of planetary interiors". The Smithosnian/NASA Astrophysics Data System (American Geophysical Union): 1–2. 
  19. ^ Edward R.D. Scott, "Impact Origins for Pallasites," Lunar and Planetary Science XXXVIII, 2007.
  20. ^ Ramsey, W.H. (April 1950). "On the Instability of Small Planetary Cores". Royal Astronomical Society 110: 325–338.  
  21. ^ a b NASA (2012). "MESSENGER Provides New Look at Mercury's Surprising Core and Landscape Curiosities". News Releases (The Woodlands, Texas: NASA): 1–2. 
  22. ^ Fegley, B. Jr. (2003). "Venus". Treatise on Geochemistry (Elsevier) 1: 487–507.  
  23. ^ Munker, Carsten; Pfander, Jorg A; Weyer, Stefan; Buchl, Anette; Kleine, Thorsten; Mezger, Klaus (July 2003). "Evolution of Planetary Cores and the Earth-Moon System from Nb/Ta Systematics". Science Reports (Science) 301 (5629): 84–87.  
  24. ^ Diamond" Planet Found; May be Stripped Star""". National Geographic (National Geographic Society). 2011-08-25 25. 
  25. ^ Bailes, M.; et al. (September 2011). "Transformation of a Star into a Planet in a Millisecond Pulsar Binary". Science Reports (Science) 333 (6050): 1717–1720.  
  26. ^ "Hot Ice Planets". MessageToEagle. 2012-04-09. 
This article was sourced from Creative Commons Attribution-ShareAlike License; additional terms may apply. World Heritage Encyclopedia content is assembled from numerous content providers, Open Access Publishing, and in compliance with The Fair Access to Science and Technology Research Act (FASTR), Wikimedia Foundation, Inc., Public Library of Science, The Encyclopedia of Life, Open Book Publishers (OBP), PubMed, U.S. National Library of Medicine, National Center for Biotechnology Information, U.S. National Library of Medicine, National Institutes of Health (NIH), U.S. Department of Health & Human Services, and, which sources content from all federal, state, local, tribal, and territorial government publication portals (.gov, .mil, .edu). Funding for and content contributors is made possible from the U.S. Congress, E-Government Act of 2002.
Crowd sourced content that is contributed to World Heritage Encyclopedia is peer reviewed and edited by our editorial staff to ensure quality scholarly research articles.
By using this site, you agree to the Terms of Use and Privacy Policy. World Heritage Encyclopedia™ is a registered trademark of the World Public Library Association, a non-profit organization.

Copyright © World Library Foundation. All rights reserved. eBooks from World eBook Library are sponsored by the World Library Foundation,
a 501c(4) Member's Support Non-Profit Organization, and is NOT affiliated with any governmental agency or department.