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Structure and evolution of the terrestrial planets

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Abstract

Geo-scientific planetary research of the last 25 years has revealed the global structure and evolution of the terrestrial planets Moon, Mercury, Venus and Mars. The evolution of the terrestrial bodies involves a differentiation into heavy metallic cores, Fe-and Mg-rich silicate mantles and light Ca, Al-rich silicate crusts early in the history of the solar system. Magnetic measurements yield a weak dipole field for Mercury, a very weak field (and local anomalies) for the Moon and no measurable field for Venus and mars. Seismic studies of the Moon show a crust-mantle boundary at an average depth of 60 km for the front side, P- and S-wave velocities around 8 respectively 4.5 km s−1 in the mantle and a considerable S-wave attenuation below a depth of 1000 km. Satellite gravity permits the study of lateral density variations in the lithosphere. Additional contributions come from photogeology, orbital particle, x-and ψ-ray measurements, radar and petrology.

The cratered surfaces of the smaller bodies Moon and Mercury have been mainly shaped by meteorite impacts followed by a period of volcanic flows into the impact basins until about 3×109 yr before present. Mars in addition shows a more developed surface. Its northern half is dominated by subsidence and younger volcanic flows. It even shows a graben system (rift) in the equatorial region. Large channels and relics of permafrost attest the role of water for the erosional history. Venus, the most developed body except Earth, shows many indications of volcanism, grabens (rifts) and at least at northern latitudes collisional belts, i.e. mountain ranges, suggesting a limited plate tectonic process with a possible shallow subduction.

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Article Open access 27 November 2015

Abbreviations

a=R e :

mean equatorial radius (km)

A(r, t) :

heat production by radioactive elements (W m−3)

A, B :

equatorial moments of inertia

b :

polar radius (km)

\(\bar b(K)\) :

complex amplitude of bathymetry in the wave number (K) domain (m)

C :

polar moment of inertia

C Fe :

moment of inertia of metallic core

C Si :

moment of inertia of silicate mantle

C p :

heat capacity at constant pressure (JK−1 mole−)

C nm,J nm,S nm :

harmonic coefficients of degreen and orderm

C/(MR 2 e ):

factor of moment of inertia

d :

distance (km)

d :

nondimensional radius of disc load of elastic bending model

D :

diameter of crater (km)

D :

flexural rigidity (dyn cm)

E :

Young modulus (dyn cm−2)

E :

maximum strain energy

ΔE :

energy loss during time interval Δt

f :

frequency (Hz)

f :

flattening

F :

magnetic field strength (Oe) (1 Oe=79.58A m−1)

g :

acceleration or gravity (cms−2) or (mGal) (1mGal=10−3cms−2)

\(\bar g\) :

mean acceleration

g e :

equatorial surface gravity

\(\bar g(K)\) :

complex amplitude of gravity anomaly in the wave number (K) domain

Δg′:

free air gravity anomaly (FAA)

Δg″:

Bouguer gravity anomaly

δg t :

gravity attraction of the topography

G :

gravitational constant,G=6.67×10−11 m3kg−1s−2

GM :

planetocentric gravitational constant

h :

relation of centrifugal acceleration (ω2 R e ) to surface acceleration (g e ) at the equator

J :

magnetic flux density (magnetic field) (T) (1T=109 nT=109 γ=104G (Gauss))

J 2 :

oblateness

J nm :

seeC nm

k (0) :

(zero) pressure bulk modulus (Pa) (Pascal, 1 Pa=1 Nm−2)

K :

wave number (km−1)

K * :

thermal conductivity (Jm−1s−1K−1)

L :

thickness of elastic lithosphere (km)

M :

mas of planet (kg)

M Fe :

mass of metallic core

M Si :

mass of silicate mantle

M(r) :

fractional mass of planet with fractional radiusr

m :

magnetic dipole moment (Am2) (1Am2=103Gcm3)

m b :

body wave magnitude

N :

crater frequency (km−2)

N(D) :

cumulative number of cumulative frequency of craters with diameters ≥D

P :

pressure (Pa) (1Pa=1Nm−2=10−5 bar)

P z :

vertical (lithostatic) stress, see also σ z (Pa)

P m n (cosΘ):

Legendre polynomial

q :

surface load (dyn cm−2)

Q :

seismic quality factor, 2πE/ΔE

Q s ,Q p :

seismic quality factor derived from seismic S-and P-waves

R=R 0 :

mean radius of the planet (km) (2a+b)/3

R e =a :

mean equatorial radius of the planet

r :

distance from the center of the planet (fractional radius)

r Fe :

radius of metallic core

S nm :

seeC nm

t :

time and age in a (years), d (days), h (hours), min (minutes), s (seconds)

T :

mean crustal thickness from Airy isostatic gravity models (km)

T :

temperature (°C or K) (0°C=273.15K)

T m :

solidus temperature

T :

sideral period of rotation in d (days), h (hours), min (minutes), s (seconds), ω=2π/T

U :

external potential field of gravity of a planet

V :

volume of planet

V p ,V s :

compressional (P), shear (S) wave velocity, respectively (kms−1)

w :

deflection of lithosphere from elastic bending models (km)

z, Z :

depth (km)

z (K) :

admittance function (mGal m−1)

α:

thermal expansion (°C−1)

η:

viscosity (poise) (1 poise=1gcm−1s−1)

Θ:

co-latitude (90°-ϕ)

λ:

longitude

ν:

Poisson ratio

ρ:

density (g cm−3)

\(\bar \rho \) :

mean density

ρ0 :

zero pressure density

ρ m , ρSi :

average density of silicate mantle (‘fluid interior’)

\(\bar \rho _{Fe} \) :

average density of metallic core

ρ t , ρtop :

density of the topography

Δρ:

density difference between crustal and mantle material

σ:

electrical conductivity (Ω−1 m−1)

σ r , σθ :

radial and azimuthal surface stress of axisymmetric load (Pa)

σ z :

vertical (lithostatic) stress (seeP z )

σII :

second invariant of stress deviation tensor

ϕ:

latitude

ω:

angular velocity of a planet (=2π/T)

ages:

in years (a), generally 0 years is present

B.P.:

before present

FAA:

Free Air Gravity Anomaly (see Δg′

HFT:

High Frequency Teleseismic event

LTP:

Lunar Transient Phenomenon

LOS:

Line-Of-Sight

NRM:

Natural Remanent Magnetization

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Contribution No. 309, Institut für Geophysik der Universität, Kiel, F.R.G.

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Janle, P., Meissner, R. Structure and evolution of the terrestrial planets. Surv Geophys 8, 107–186 (1986). https://doi.org/10.1007/BF01902412

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