Evolution of giant gaseous protoplanets embedded in the primitive solar nebula

Details Evolution of giant gaseous protoplanets embedded in the primitive solar nebula Evolution of giant gaseous protoplanets embedded in the primitive solar nebula

Mar 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982icar...49..298c&link_type=abstract

Icarus, vol. 49, Mar. 1982, p. 298-312.

Astronomy and Astrophysics

Astronomy

21

Gas Giant Planets, Planetary Evolution, Protoplanets, Solar Corona, Astronomical Models, Terrestrial Planets, Time Dependence

Scientific paper

In contrast to earlier evolutionary calculations, which assumed that protoplanets are isolated, the present spherically symmetric approximation for a protoplanet of one Jovian mass during the early phase of quasi-static contraction invokes a time-dependent surface boundary condition that simulates physical conditions in an evolving primitive solar nebula. Assuming in a first set of calculations that the protoplanet is surrounded by a thermal bath whose temperature varies with time, and whose pressure is small and constant, results show evaporation and complete dispersal of the object. A second set of calculations varies both temperature and pressure at the surface with time, according to solar nebula models, and yields an acceleration or retardation of evolution, relative to that of an isolated protoplanet, depending on the relative entropy of the nebula and the protoplanet's outer layers. Processes by which terrestrial planets can form in the cores of giant gaseous protoplanets are discussed.

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