Numerical models of the primitive solar nebula.

摘要: Abstract Numerical models have been constructed to represent probable conditions in the primitive solar nebula. A two mass fragment of a collapsing interstellar gas cloud has represented by uniformly rotating sphere. Two cases considered: one which internal density sphere is uniform and other falls linearly from central value zero at surface (the linear models). These assumptions served define distribution angular momentum per unit with fraction. The spheres were flattened into disks, disks found there was force balance radial vertical directions, subject certain approximations, everywhere assigned values mass. pressure gradient included balance. energy transport direction involved convection radiative equilibrium; principal contributors opacity lower temperatures metallic iron grains ice. contained zones, an inner due dissociation hydrogen molecules, outer high grains. characteristic semithickness ranged about 0.1 astronomical units near center exterior. Characteristic times radiation lifetimes for these initial nebula estimated. Both types lifetime as short few years part models, became 104 or longer distances greater than ten units.