384 



T. C. CHAMBERLIN 



may be regarded as performing a semi-revolution about each 

 other. By the terms of the special case in hand, this semi-revo- 

 lution must be performed in a very few hours. During these 

 few hours the gaseous body {^A) is undergoing elongation at a 

 rate not much less than that represented by its full explosive 



Fig. I. — Diagram illustrating the elongating and rotatory effects of a solid 

 stellar body, B, upon a gaseous sun, A, during their mutual approach to periastron. 

 ^1,2, 3. 4.^5 indicate successive positions, changes of form, and rotation of the gaseous 

 star on its approach to periastron. j5 ^' =^•3"'"' 5 represent the successive positions of 

 a solid body of equal mass and velocity which is assumed for convenience to remain 

 intact. Position A'^ corresponds to B^, A^ to £", etc. The lines' joining their cen- 

 ters indicate the successive directions of mutual attraction. The arrows indicate 

 direction of movement. 



competency. The rotational forces are diagrammatically illus- 

 trated in Fig. I, in which the lag is merely estimated and the 

 distortion of A is simplified while that of B is neglected. 



