Physics
Scientific paper
Jun 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979pepi...19..168s&link_type=abstract
(Lunar and Planetary Institute and NASA, Workshop on Solid Convection in the Terrestrial Planets, Moffett Field, Calif., Dec. 12
Physics
23
Formations, Planetary Cores, Planetary Evolution, Planetary Structure, Terrestrial Planets, Thermal Energy, Conductive Heat Transfer, Dynamo Theory, Ohmic Dissipation, Planetary Gravitation, Planetary Mantles, Planetary Radiation, Planetology, Radioactivity, Temperature Profiles, Core, Earth, Moon, Mercury, Venus, Mars, Chronology, Gravity, Heat, Radioactivity, Thermal History, Dynamo Theory, Size, Models, Volume, Differentiation, Mass, Density, Metals, Topography, Freezing, Mantle, Convection, Pressure, Ch
Scientific paper
The size, evolution and energetics of the earth's core and the probable central, metalic cores of Mercury, Venus, the moon and Mars are discussed. The cores of Mercury, Mars and the earth are considered likely to decrease in relative mass and volume with distance from the sun; the moon does not fit this sequence and data from Venus are insufficient. Core formation is concluded to have occurred early (prior to four billion years ago) on the earth and Mercury, while that on the moon would have occurred over a longer interval and the core of Mars would have formed much later. Of the possible energy sources in planetary cores able to maintain a molten state and drive magnetic dynamos, the energy of core formation was probably spent too early in planetary history to provide much present power, and the energy gained from freezing an inner core in the earth and Mercury are considered at best marginally able to match conductive heat loss. Future measurements proposed to improve the quantitative understanding of core properties include a better documentation of the magnetic fields of Venus and Mars and the seismometry of Mars.
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