Physics – Condensed Matter
Scientific paper
Feb 1975
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975phdt.........3p&link_type=abstract
Ph.D. Thesis Yeshiva Univ., New York, NY.
Physics
Condensed Matter
4
Planetary Evolution, Solar Corona, Adiabatic Conditions, Astronomical Models, Cores, Gravitational Fields, Helium, Hydrogen
Scientific paper
When a planet core composed of condensed matter is accumulated in the primitive solar nebula, the gas of the nebula becomes gravitationally concentrated as an envelope surrounding the planetary core. Models of such gaseous envelopes were constructed subject to the assumption that the gas everywhere is on the same adiabat as that in the surrounding nebula. The gaseous envelope extends from the surface of the core to the distance at which the gravitational attraction of core plus envelope becomes equal to the gradient of the graviational potential in the solar nebula; at this point the pressure and temperature of the gas in the envelope are required to attain the background values characteristics of the solar nebula. In general, as the mass of the condensed core increases, increasing amounts of gas become concentrated in the envelope, and these envelopes are stable against hydrodynamic instabilities.
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