On the Chemistry of the Hottest Stars, 149 



VI. Comparison of the metallic results with those given by the cleveite gases and 

 hydrogen. 



The cleveite gases. 

 Hydrogen. 



VII. Temperature ranges of the metallic and cleveite lines. 



The lower limit in the case of the enhanced metallic lines. 

 The upper limit in the case of the enhanced metallic lines. 

 The cleveite gases. 

 General conclusions. 



Till. Inversion of the phenomena on cooling in the case of the metallic and cleveite 

 lines. 



The temperature curve. 

 Metallic results, descending. 

 Cleveite gas results. 



IX. On the absorbing conditions on the upivard and downward sides of the tem- 

 perature curve. 



Temperature order of some of the hottest stars on the two sides of the 



temperature curve. 

 The absolutions not identical. 

 The new criteria. 



General conclusions as to the spectroscopic differences on the two sides of 

 the curve. 



The probable physical causes of the differences. 

 X. Are we in presence of the highest stellar temperatures ? 



Paet II. 



of the new results on the dissociation hypothesis. 



Historical statement. 

 Special reference to solar work. 

 Some special experiments. 



The main points. 



Flutings represent vibrations of complex molecules. 

 The complexity of the line spectrum. 

 The effect of pressure on wave-length. 

 The question of series. 

 Statement of some opinions. 

 The basic lines. 



§ III. Extension of the field of investigation. 

 A possible objection. 



The connection between chromosphere and stellar phenomena. 



The possible action of heat on the sun's present chromosphere. 



The Orion stars. 



The law of continuity. 



The ultimate molecules involved. 



Prout's hypothesis. 



Final result. 



XII. General Conclusions. 



M 2 



XI. Bearing 

 SI. 



