Physics
Scientific paper
Apr 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979e%26psl..43...22h&link_type=abstract
Earth and Planetary Science Letters, vol. 43, no. 1, Apr. 1979, p. 22-28.
Physics
34
Dense Plasmas, Melting, Primitive Earth Atmosphere, Protoplanets, Atmospheric Temperature, Blankets, Deposition, Hydrostatic Pressure, Opacity, Planetary Mass, Planetary Nebulae, Temperature Distribution
Scientific paper
When the proto-earth was growing by the accretion of planetesimals and its mass became greater than about 0.1 present-earth mass, an appreciable amount of gas of the surrounding solar nebula was attracted toward the proto-earth to form an optically thick, dense atmosphere. The structure of this primordial atmosphere is studied under the assumptions that (1) it is spherically symmetric in hydrostatic equilibrium, and (2) the net energy outflow (i.e., the luminosity) is constant throughout the atmosphere. The results of calculations show that the temperature at the bottom of the atmosphere, namely, at the surface of the proto-earth increases greatly with the mass of the proto-earth and it is about 1500 K for a proto-earth mass of 0.25 present-earth mass. This high temperature is due to the blanketing effect of the opaque atmosphere. Thus, as long as the primordial solar nebula was existing, the surface temperature of the proto-earth was kept high enough to melt most of the materials and, hence, the melted iron sedimented towards the center to form the earth's core.
Hayashi Chuichiro
Mizuno Hideki
Nakazawa Kazuhiro
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