348 



o 



0,0017' A, for paira of lines whose average distance amoniits to 

 1,7 times their mean width.') This harmonizes, as regards order 

 of magnitude, with liie computed value. 



In the publication just referred to we have shown that the mutual 

 repulsions which two equal, symmetrical lines seem to exercise on 

 each otliei' as a mere consequence of systematic (photograpliical or 

 psychological) errors of measurement, only become appreciable when 

 the distance between the lines sinks below 1,5 times their width, 

 and that, therefore, only a fraction of the mutual influence observed 

 with Fraunhofer lines, can be ascribed to sucii errors. 



The theoretical anticipation here advanced thus proves to be 

 consistent with the observational material till now available; but 

 for the present our conclusion cannot go beyond this, because the 

 quantities involved in this investigation are near the limit of preci- 

 sion attainable with existing means for measurement in the solar 

 spectrum. 



Utrecht, April 1923. Heliophysical Institute. 



') Gf. our article .Kritisches zu Deutungen des Sonnenspektruras", Ann. d. 

 Phys. 71, p. 50, 1923. 



