Local condensations in collisional discs

Details Local condensations in collisional discs Local condensations in collisional discs

Feb 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987em%26p...37..113h&link_type=abstract

Earth, Moon, and Planets (ISSN 0167-9295), vol. 37, Feb. 1987, p. 113-131.

Statistics

Computation

Computational Astrophysics, Condensation, Planetary Evolution, Solar System, Clouds, Disks, Equilibrium, Particle Motion

Scientific paper

The equations for a collisional disc permit solutions which represent small local condensations of matter in a uniform medium. With parameter values appropriate to the pre-planetary disc the clouds are 50 to 1500 times as dense as the surrounding region and have a mass of 1014 to 1015g. The formation of clouds follows from collisional instability. They maintain their equilibrium by means of a mass exchange with the adjacent matter. The clouds are proposed to replace the solid planetesimals in the theory of planetary formation.

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