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The Evolution of a Gravitating, Rotating, Condensing Fluid
Excerpt from The Evolution of a Gravitating, Rotating, Condensing Fluid
From this line of reasoning it has been regarded as probable that celestial masses, through loss of heat and consequent contraction, do break up in this way Often enough to make the process an important one in cosmogony. It is a commonly accepted theory that the sun and planets once existed as nebulae and that they, as well as the stars, developed from matter in a state Of wide distribution. The problem presented by them in this condition is that of separate discrete particles possessing individual velocities and subject to accelerations produced by the force of gravitation due to their mutual attractions. It is essentially the prob lem Of the orbital motion Of n bodies, and as such must con form to the laws expressed by the general equations deduced for such motion. I shall therefore regard a star, or the sun, as presenting the n body problem in which motions are modified and energy produced by the impacts to which the n bodies are subject. In a general discussion of the problem, it would be necessary to consider masses Of all sizes, such as might be encountered in nebulae, but when the configuration Of particles has attained to the state Of a star or the sun the n bodies with which we have to deal, will be the smallest divisions Of matter, Â namely, molecules. Whatever the masses composing the sun may have been when it was in a state Of wide distribution, continued impact would tend to divide them into the smallest divisions of matter which can exist by themselves. The motion of the center Of mass may be considered equal to zero since in the present problem we are concerned only with the evolution Of n bodies with respect to it. We are thus led to an immediate consideration Of the three integrals of area which are expressed by the following equations7'
From this line of reasoning it has been regarded as probable that celestial masses, through loss of heat and consequent contraction, do break up in this way Often enough to make the process an important one in cosmogony. It is a commonly accepted theory that the sun and planets once existed as nebulae and that they, as well as the stars, developed from matter in a state Of wide distribution. The problem presented by them in this condition is that of separate discrete particles possessing individual velocities and subject to accelerations produced by the force of gravitation due to their mutual attractions. It is essentially the prob lem Of the orbital motion Of n bodies, and as such must con form to the laws expressed by the general equations deduced for such motion. I shall therefore regard a star, or the sun, as presenting the n body problem in which motions are modified and energy produced by the impacts to which the n bodies are subject. In a general discussion of the problem, it would be necessary to consider masses Of all sizes, such as might be encountered in nebulae, but when the configuration Of particles has attained to the state Of a star or the sun the n bodies with which we have to deal, will be the smallest divisions Of matter, Â namely, molecules. Whatever the masses composing the sun may have been when it was in a state Of wide distribution, continued impact would tend to divide them into the smallest divisions of matter which can exist by themselves. The motion of the center Of mass may be considered equal to zero since in the present problem we are concerned only with the evolution Of n bodies with respect to it. We are thus led to an immediate consideration Of the three integrals of area which are expressed by the following equations7'
353 pages, Paperback
First published July 21, 2015
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