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Distribution Of Planetary Systems

  • T. V. Ruzmaikina
Conference paper
Part of the Astrophysics and Space Science Library book series (ASSL, volume 144)

Abstract

Planets are formed in the gas-dust protoplanetary disc surrounding the solar type star at early stage of its evolution. The star and disc originate as a result of collapse of a cloud which angular momentum J is small enough to form a star-like core of minimal mass in the center of the cloud. However, the angular momentum must exceed the maximal angular momentum admissible for the formation of a single star. This puts the following limits on the cloud’s angular momentum:
$$10^{51} \leqslant \text{J} \leqslant 210^{51} \text{ g cm}^2 \text{ s}^{ - 1}$$
The ability of planetary systems depends on the number of protostellar clouds having the angular momenta within this interval. The rotation of dark cores in the clouds comes from the interstellar turbulence. The turbulence is intermittent over the scales less than O.lpc. The study of observational data on the rotation of the dark cores in molecular clouds shows that a fraction from 10−4 up to ≥ O.l of all clouds have the appropriate angular momenta. Thus, a fraction of stars having the planetary systems can amount to o.l of all stars of solar mass in the Galaxy.

Keywords

Angular Momentum Molecular Cloud Planetary System Solar Nebula Solar Mass 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© Kluwer Academic Publishers 1988

Authors and Affiliations

  • T. V. Ruzmaikina
    • 1
  1. 1.Academy of SciencesSmidt Institute of the Physics of EarthMoscowUSSR

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