164 Trans. Acad. Sci. of St. Louis. 



the mass of the sun is 2.18 X 10^ grammes. This is about 

 2000 times the mass computed from (17)'. 



The conditions here discussed, may perhaps be brought 

 about in some such way as this. An infinitely diffused mass 

 of gas occupies an infinite space. It is surrounded by an in- 

 finite series of infinite spaces, having perhaps an increasingly 

 higher order of magnitude. A great meteorite, or a world, 

 strays into the nebula, and probably sets it into rotation. The 

 nebulous mass gravitates towards the solid nucleus, which has 

 been already slightly warmed by f rictional contact with the 

 diffused gas. As the gravitating action continues, the tem- 

 perature rises, and the solid mass, while still remaining solid, 

 becomes also a liquid and a gas. The bounding surface 

 between solid and gas has disappeared. How else can gaseous 

 pressure develop in an infinitely diffused mass of gas having a 

 temperature at which all gases are solid? 



This pressure thus developed, is automatically applied in a 

 perfectly definite way, as radiation and contraction proceed. 

 If, as the temperature rises, the heat radiates more and 

 yet more rapidly, the operation is thereby hastened, but the 

 law of contraction remains unchanged. The relations between 

 P, 3, and Tmust remain invariable. 



These equations are now in condition to be linked with the 

 solar radiation constant, and the time element. They may 

 thus serve to permit a re-examination of the history of the 

 evolution of the solar system. 



lisued October 1, 1903. 



