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Terrestrial Planets

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Planets, Stars and Stellar Systems

Abstract

The four terrestrial planets (Mercury, Venus, Earth, and Mars) and Earth’s Moon display similar compositions, interior structures, and geologic histories. The terrestrial planets formed by accretion ∼ 4.5 Ga ago out of the solar nebula, whereas the Moon formed through accretion of material ejected off Earth during a giant impact event shortly after Earth formed. Geophysical investigations (gravity anomalies, seismic analysis, heat flow measurements, and magnetic field studies) reveal that all five bodies have differentiated into a low-density silicate crust, an intermediate density silicate mantle, and an iron-rich core. Seismic and heat flow measurements are only available for Earth and its Moon, and only Earth and Mercury currently exhibit actively produced magnetic fields (although Mars and the Moon retain remanent fields). Surface evolutions of all five bodies have been influenced by impact cratering, volcanism, tectonism, and mass wasting. Aeolian activity only occurs on bodies with a substantial atmosphere (Venus, Earth, and Mars) and only Earth and Mars display evidence of fluvial and glacial processes. Earth’s volcanic and tectonic activity is largely driven by plate tectonics, whereas those processes on Venus result from vertical motions associated with hotspots and mantle upwellings. Mercury displays a unique tectonic regime of global contraction caused by gradual solidification of its large iron core. Early large impact events stripped away much of Mercury’s crust and mantle, produced Venus’ slow retrograde rotation, ejected material off Earth that became the Moon, and may have created the Martian hemispheric dichotomy. The similarities and differences between the interiors and surfaces of these five bodies provide scientists with a better understanding of terrestrial planet evolutionary paths.

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Abbreviations

ASTER :

Advanced Spaceborne Thermal Emission and Reflection radiometer

ESA :

European Space Agency

Ga :

Giga-years (billion years, or 109 years)

JHU APL :

Johns Hopkins University Applied Physics Laboratory

JPL :

Jet Propulsion Laboratory

KREEP :

Potassium (K), Rare Earth Element, and Phosphorus rich lunar rocks

KT :

Cretaceous-Tertiary

LCROSS :

Lunar CRater Observation and Sensing Satellite

LHB :

Late Heavy Bombardement

LPI :

Lunar and Planetary Institute

LRO :

Lunar Reconnaissance Orbiter

Ma :

Million years (106 years)

MESSENGER :

MErcury Surface, Space ENvironment, GEochemistry, and Ranging

MFF :

Medusae Fossae Formation

MGS :

Mars Global Surveyor

MOLA :

Mars Orbiter Laser Altimeter

MSSS :

Malin Space Science Systems

NASA :

National Aeronautics and Space Administration

PLD :

Polar layered deposits

SELENE :

SELenological and ENgineering Explorer

SMART-1 :

First Small Missions for Advanced Research and Technology

SNC :

Shergottites, Nakhlites, and Chassignites (Martian meteorites)

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Authors and Affiliations

  1. Department of Physics and Astronomy, Northern Arizona University, NAU Box 6010, 86011-6010, Flagstaff, AZ, USA

    Dr. Nadine G. Barlow

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  1. Dr. Nadine G. Barlow
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Editors and Affiliations

  1. Department of Physics & Space Sciences, Florida Institute of Technology, University Boulevard, Melbourne, FL, USA

    Terry D. Oswalt

  2. Professor of Physics and Physics Department Chair, Wesleyan University, IL, USA

    Linda M. French

  3. Astronomy Department, University of California, Berkeley, CA, USA

    Paul Kalas

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Barlow, N.G. (2013). Terrestrial Planets. In: Oswalt, T.D., French, L.M., Kalas, P. (eds) Planets, Stars and Stellar Systems. Springer, Dordrecht. https://doi.org/10.1007/978-94-007-5606-9_3

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