Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...309..301s&link_type=abstract
Astronomy and Astrophysics, v.309, p.301-312
Astronomy and Astrophysics
Astrophysics
49
Accretion Disks, Solar System: Formation
Scientific paper
The problem of planetary system formation and its subsequent character can only be addressed by studying the global evolution of solid material entrained in gaseous protoplanetary disks. We start to investigate this problem by considering the space-time development of aerodynamic forces that cause solid particles to decouple from the gas. The aim of this work is to demonstrate that only the smallest particles are attached to the gas, or that the radial distribution of the solid matter has no momentary relation to the radial distribution of the gas. We present the illustrative example wherein a gaseous disk of 0.245Msun_ and angular momentum of 5.6x10^52^g.cm^2^/s is allowed to evolve due to turbulent viscosity characterized by either α=10^-2^ or α=10^-3^. The motion of solid particles suspended in a viscously evolving gaseous disk is calculated numerically for particles of different sizes. In addition we calculate the global evolution of single-sized, non-coagulating particles. We find that particles smaller than 0.1cm move with the gas; larger particles have significant radial velocities relative to the gas. Particles larger then 0.1cm but smaller than 10^3^cm have inward radial velocities much larger than the gas, whereas particles larger than 10^4^cm have inward velocities much smaller than the gas. A significant difference in the form of the radial distribution of solids and the gas develops with time. It is the radial distribution of solids, rather than the gas, that determines the character of an emerging planetary system.
Stepinski Tomasz F.
Valageas Patrick
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