ASTR 1210 (O'Connell) Study Guide

A. Uniqueness

• Largest terrestrial planet

• Has largest satellite with respect to its own diameter (see images in Guide 13)

• Large atmospheric abundance of water is unique among terrestrials

• Open oceans: unique in solar system; water covers 2/3 of surface

• O₂-rich atmosphere (21% by volume)

• Life! Living organisms cover the Earth.
  There is no definite evidence yet for any other biospheres in the solar system. If these exist, the lifeforms are likely to be primitive. See Guide 23.

B. The Earth's Biosphere

• Consists of Earth's crust, oceans, lower atmosphere:
  
  • Thin!. See this picture.

  • For a scale model: Take a piece of paper. Fold once. Paste on a basketball. A thin smear of lifeforms on a huge sphere.

• Fragile!
  • We live in a delicate balance with nature

  • In cosmic time, our favorable ecosystem is transient and evolving rapidly.
    • For example: Earth's surface, as hard and unchanging as it may seem, is only temporary.

  • Although the rapidly growing human population (see Study Guides 9 and 19) is having deleterious effects on the biosphere, these are survivable (even if the costs could be catastrophic). The most serious, long-term threats to the ecosystem are extraterrestrial and beyond immediate human control: asteroid/comet impacts, solar evolution, supernovae and other stellar explosions, etc.

  • Astronomy is the ultimate ecology.

Sedimentary Layers in the Walls of the Grand Canyon (Reiner Stenzel)

C. The Age of the Earth

• Sedimentation rate/geological strata method
  • Developed in 19th century

  • The rock layers of, e.g., the Grand Canyon were once under water. They are hardened sediment that settled to the floors of ancient seas, deposited over long periods of time by rivers that flowed into the oceans. Among other things, the sedimentary layers can contain fossils of ancient plants and animals. They can also harbor processed organic material in the form of oil and natural gas.

  • Age-dating based on stratigraphy makes use of the relatively uniform rate of sediment deposition to estimate the age of different stata. Deeper layers are older. For an example of dating of the Grand Canyon, click on the picture above. "Bio-stratigraphy" uses embedded fossils to refine ages.

  • These methods are not very precise, but they were sufficient to prove to 19th century geologists that the Earth's surface had evolved over millions of years of time. They are still very important in determining the relative ages for different rock formations, which can be traced across huge geographical areas.

• Radioisotope (or "radiometric") dating method
  • This is based on the well-determined decay rates of naturally occurring radioactive ("unstable") isotopes, e.g. uranium ==> lead. It is much more precise than stratigraphy, and the basic mechanism is thoroughly understood on the basis of quantum mechanics. It can be applied to rock samples obtained anywhere on the Earth or elsewhere in the solar system (e.g. from the Moon or meteorites).

  • The "half life" of an unstable isotope is the time it takes for half of the original sample to decay to a "daughter" isotope. See this Java Applet illustrating the decay process. Half lives for unstable isotopes are determined by the structure of their nuclei and range from microseconds to billions of years.

  • Method: first, chemically separate parent from daughter isotopes; then estimate the age from the ratio of parent to daughter.
    "Carbon-14" dating is the best known type of radiometric dating. Because the half-life of ¹⁴C is only 5570 years, it is very important for studies of historical and pre-historical human artifacts; but it is not useful for geological time scales.
    For time scales up to billions of years, dating schemes using decay chains such as uranium-lead or rubidium-strontium are used. These can yield a dating precision in the range of 0.1-2%.

• Results
  • Oldest Earth surface rocks: 3.9 billion years (a few samples of zircon crystal date to 4.4 Byr)

  • Moon, meteorites: 4.5-4.6 billion years
    The oldest Earth rocks are younger than those of the Moon, even though the Earth probably formed somewhat earlier than the Moon, because the Earth's surface has been recycled by plate tectonics.

  • Earth chronologies (click):
    Geological/Fossil Chronology
    Geological Chronology#1
    Geological Chronology#2

Cross-section through the Earth (USGS)

D. Earth's Interior

• Earth's mass is determined from the orbit of the Moon or of artificial spacecraft by applying Kepler's 3rd law.
  • Reminder: the Earth's mass can not be determined from its orbit around the Sun (see Study Guide 8).

• The density = Mass/Volume of a planet is an essential clue to its composition
  • Earth 5.5 grams/cc ==> heavier elements (like Si,O,Fe)

  • Jupiter 1.3 grams/cc ==> lighter elements (H,He)

  
• Probe interior with seismic waves from earthquakes
  • These show that the interior is differentiated: i.e. composition and density change with depth

  • 3 main zones: Core (innermost), mantle (body), crust (outermost).
    (See illustration above.)

  • Densities range from 12 grams/cc in the core to 3 grams/cc in the crust, implying that the core contains more heavy elements than the crust.

  • Temperature at the core is over 5000 K.

• The differentiation implies that Earth's interior was once molten, so that heavier materials could settle to the center.
  • Initial heat source: impacts of infalling planetesimals during formation stages. Further heat released during differentiation, as heavier materials sink.

  • Continuing (billions of years) interior heat source: radioactive decay of uranium and other materials. Even though only a small fraction of the Earth's makeup, the heat generated by decay of these materials escapes only slowly, so the interior remains molten/plastic.

• Heat transfer/cooling
  • Interior heat escapes from planets through their surfaces. Heat is transferred by several processes:
    Conduction: transfer of energy by contact at the molecular level from hotter to cooler regions.
    Convection: transfer of energy by actual motions of material. These "convection currents" systematically deposit heat at shallower depths.

  • As long as the interior retains significant heat, its transfer to the surface drives various forms of "geological activity" (see next section). Convection currents are also responsible for producing a magnetic field extending into space.

E. "Plate Tectonics"

• A new (1950's - 60's) "paradigm" for the origin of geological structures. Click here for the history of plate tectonic interpretations.

• The outer layers of the Earth (the crust and the upper mantle, together called the lithosphere) are thin and cracked into pieces called "plates" (diagram above). These float on the partially melted, plastic material (the asthenosphere) below them.

• The plates move in response to the slow convection currents in the mantle.
  Convection circulation includes rising warm material and falling cool material. It is driven by the temperature gradient within the Earth.
  Typical motions are very small, about 1 cm per year. This sounds ridiculously tiny, but such motions can now be easily measured with technologies similar to those of the GPS system.
  On geological time scales such motions have drastic cumulative effects, as plates collide with each other or are exchanged with the mantle. Over 100 million years (a short time geologically), a motion of 1 cm per year adds up to 1000 km.

  
• Plate motion or "continental drift" is responsible for all the geological activity on the Earth's surface: mountain building, rifting, earthquakes, vulcanism (as at right), etc.

• Earthquakes and vulcanism are concentrated primarily at the periphery of plates where two plates are moving against each other (e.g. the "Pacific Ring of Fire", see the map above). Young mountain ranges (e.g. the Andes and Himalayas) are also found at the edges of plates.

• The Earth's surface is being continuously recycled. Older plates are pushed back into the interior and melted while newer materials are added to the surface in upwelling zones. Melting of plates gassifies some of their materials and cycles those back into the atmosphere.

• Earth is the only terrestrial planet with continuous, large-scale tectonics

• Illustrations:
  Continental drift animation (small)
  Continental drift animation (large)
  Building the Himalayas
  Maxi-Tsunami Simulation: This shows the tidal wave threat from a possible "flank collapse" of the Kilauea volcano in Hawaii. [Note: the Hawaiian volcanoes are produced by a concentrated plume of hot magma rising from the interior rather than by plate collisions. This is the same kind of mechanism that produced the Tharsis volcanoes on Mars.]

Earth's Atmosphere From Orbit

F. Atmosphere

• The original atmosphere was "outgassed" from the interior soon after Earth formed.

• There has been strong evolution of the constituents of the atmosphere over time
  Many different physical processes drive atmospheric evolution for the terrestrial planets. A pictorial summary is given here.
  These and their consequences for Earth, Venus, and Mars will be discussed further in Study Guide 19.

• Earth's atmosphere is now predominantly N₂, and O₂. This is unlike the atmospheres of Venus and Mars (which are mainly CO₂) and unlike the early Earth atmosphere.

• O₂ is directly linked the the presence of life on Earth. It is produced mainly by photosynthesis in plants and started rapidly increasing in the atmosphere about 500 million years ago. Since it is so reactive, free O₂ cannot persist in an atmosphere without life.

• The temperature at any height is determined by the balance of heating against cooling.

• Circulation (wind) is driven by heating (near equator) vs. cooling (near poles) and by effects of Earth's rotation (the "coriolis effect")

Bennett textbook: Secs. 8.5, 9.1, 9.6
Study Guide 12

Bennett textbook: Secs. 9.2, 9.3, 10.3
Study Guide 13

Introductory Course on Earth Systems (J. Schieber, Indiana U)
Tutorial on Remote Sensing and Earth Geology (Federation of American Scientists)
More Information on Age-Dating the Earth (Pogge, OSU)
Radiometric Dating (Wikipedia)
Stratigraphy (Wikipedia)
Brandt's Evolutionary/Geological Timeline
The Geologic Time Scale (USGS)
Geological and Biological Timelines (San Diego Natural History Museum)
Geochronology Methods (USGS)
Carbon-14 Dating
Dynamic Earth (Univ. of Leeds)
Background Information on Plate Tectonics (UC Berkeley)
More Background Information on Plate Tectonics (USGS)
The Electronic Volcano
Background Information on the Structure & Chemistry of the Atmosphere
Views of the Earth's atmosphere from space (O'Connell)

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Last modified March 2013 by rwo

Drawing of seismic waves from ASTR 161 University of Tennessee. Text copyright © 1998-2013 Robert W. O'Connell. All rights reserved. These notes are intended for the private, noncommercial use of students enrolled in Astronomy 1210 at the University of Virginia.