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Surface Science of the Terrestrial Planets

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Solar System Astrophysics

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Abstract

In this chapter we explore the surfaces as well as the interiors of Mercury, Venus, and Mars, and compare their properties to those of the Earth and Moon, which we have already examined. In Milone and Wilson (2013, Chap. 10), we study the nature of atmospheres and ionospheres with tools of physics and chemistry; in Chap. 11 we consider the magnetospheres.

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Notes

  1. 1.

    Pluto, which is smaller than Mercury and the Earth’s moon, and may not be the largest icy body beyond the orbit of Neptune in the outer solar system, was reclassified as a “dwarf planet” by the International Astronomical Union in 2006 (see Milone and Wilson 2014, Chaps. 13–16).

  2. 2.

    The geometric albedo is defined in the Astronomical Almanac as the ratio of the illumination of the planet at zero phase angle (i.e., the brightness as viewed from the light source) to that of a pure white Lambert plane surface (or Lambertian surface) of the same radius and position as the planet. A Lambert plane surface is one for which the reflected radiant intensity (or the reflected luminous intensity), I, is directly proportional to the cosine of the angle, θ, between the observer’s line of sight and the surface normal: I(θ) = I(0) cos θ.

  3. 3.

    The word “tectonic” refers to any geologic process which involves the movement of solid rock. Large-scale tectonics in the crust generally is caused by processes in the underlying mantle. In plate tectonics on the Earth, solid lithospheric plates slide around on the surface in response to convection in the mantle. Plate tectonics does not seem to occur on Venus, but other tectonic processes do.

  4. 4.

    For a more general discussion of this principle, see Milone and Wilson 2014, Sect. 10.2.2.

  5. 5.

    Tectonic: pertaining to (or caused by or resulting from) structural deformation of the crust.

  6. 6.

    Fossa is the Latin word for a ditch or trench. Fossae is the plural. See Figs. 9.33 and 9.34 for examples on Mars.

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Authors and Affiliations

  1. Dept. Physics & Astronomy, University of Calgary, Calgary, Alberta, Canada

    Eugene F. Milone (Professor Emeritus) & William J. F. Wilson (Senior Instructor Emeritus)

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  1. Eugene F. Milone
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  2. William J. F. Wilson
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Challenges

Challenges

  1. [9.1]

    The root-mean-square (rms) speed, v rms, of atoms or molecules of mass m in a gas in thermal equilibrium at temperature T is given by the equation 1/2 m(v rms)2 = (3/2)kT, where k is Boltzmann’s constant (Milone & Wilson 2014, Sect. 10.1). If these atoms or molecules are a component of a planetary atmosphere, then this component escapes into space over a timescale of weeks if v rms = 1/3 v esc, where v esc is the escape velocity from the planet [equation (5.39)]; 104 years if v rms = 1/4 v esc, and 108 years if v rms = 1/5 v esc, Calculate (a) the escape velocity of an atom from the surface of Mercury and (b) the rms speeds of atoms of S and Fe vapor in thermal equilibrium with the surface of a magma ocean at a temperature of (i) 1,000 K; (ii) 1,500 K on the planet Mercury. (c) For each of these temperatures, comment on the retention of these atoms by Mercury if the ocean surface is molten for 105 years.

  2. [9.2]

    Compute the impact speed and specific impact energy for an asteroid colliding with each of the terrestrial planets and the Earth’s moon. Assume the asteroid to have an orbit with the same semi-major axis as the orbit of the planet.

  3. [9.3]

    Ignore atmospheric effects for the situation in [9.2] and comment on the size of the craters one would expect for each body for the same mass of impactor of a stony meteorite (say ρ = 3,500 kg/m3). Is it reasonable to suppose one should ignore atmospheric effects?

  4. [9.4]

    Estimate the mass of impactor required to create the Hellas basin on Mars. Show all reasoning.

  5. [9.5]

    Compare the observed and global equilibrium temperature of Venus. Is it reasonable to ignore internal heat sources on this planet? If the only source of heat on Venus were internal, compute its equilibrium temperature.

  6. [9.6]

    Solar evolution models suggest that the Sun will be 10 % more luminous ~1 Gy from now. If it were so, how would this affect the environments of Earth and Mars at that stage?

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Milone, E.F., Wilson, W.J.F. (2014). Surface Science of the Terrestrial Planets. In: Solar System Astrophysics. Astronomy and Astrophysics Library. Springer, New York, NY. https://doi.org/10.1007/978-1-4614-8848-4_9

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