737 



lias calculated for the equilibri inn-forms of spherical cosmic gaseous 

 masses (for )i=V/^, k=iA): the integration has been performed 

 by mechanical quadrature. The integration-intervals were taken four 

 times smaller than the unit of r, as iised by Emdkn ; expressed in 

 our unit the radius of the exterual surface is 21.67. The result of 

 the integration was as follows: 



^Q rdr 



The integral I is proportional to the temperature. The result theie- 

 fore shows, that the ?nu'fonn expansion requires a distrihuiion of 

 temperature inkich differs very little from an even temperature 

 tfiroughout the mass. If the original process is not a rise of temperature 

 at the surface by friction in a nebulous mass, but if thi'ough some 

 catastrophe the entire uiass becomes hot throughout, an approximately 

 equal temperature through the whole mass might be expected and 

 in that case, as was here shown, an approximately uuiform expansion 

 would take place. 



Now for 



i = 



21.67 o 



9 



11 Cr. '1^ 



R 



(8) 



we liave 



7' = 



IR*A^ 



lR'A'(ji 



21,67'.// 21,67'.8,3.10" 

 if // is the molecular weight of the gas of which the star consists. 

 Substituting the value of A found above, the mean temperature 

 (taking 1=25) becomes: 



25 X 6.25.10-12 



2' — — -— — /r 



21,67' X 8,8.10' 



(J = 4. 10-21 fi^^i 



(9) 



48 



Proceedings Royal Acad. Amsterdam. Vol. XXI. 



