122 Scientific Intelligence. 
fact that the F line widens as it approaches the sun, the bright 
line appearing sometimes to extend upon the sun itself, sometimes 
on one side of the dark F line and sometimes upon the other. Dr. 
Frankland and Mr. Lockyer believe that they have owl that the 
widening of the F line is due to pressure, and not to temperature 
er not 
e 
Lockyer found that the bright F line underwent strange contor- 
tions, as if there were some iturbing cause which varied the re- 
frangibilit of the line. At the same time and in the same protu- 
berance characteristic lines of barium, magnesium, nickel (?) and 
some unknown substance were observed. In this case, therefore, 
there was an n apenas from the SER into the chromosphere, 
accompanying which there were changes of enormous magni itude 
in the prominence, and when the apninh ceased the prominence 
away. In a subsequent paper Mr. Lockyer communicated 
not very far from the sun’s limb. The author’s results, in his own 
words, are as follows: 
L. Under certain conditions, the C and F lines may be observed 
bright on the sun, and in the spot-spectrum also, as in prominences 
or in the chromosphere. 
Il. Under certain conditions, although they are not observed as 
bright lines, the corresponding Fraunhofer lines are blotted out. 
he accompanying changes of refrangibility of the lines in 
question show that the absorbing material moves upward and 
downward as regards the r radiating material, and that these mo- 
tions may be observed with considerable accurac 
, IV. The bright lines observable in the ordinary spectrum are 
sometimes interrupted by the spot-spectrum, 7, ¢., they are only vis- 
ible in those parts of the solar spectrum near, and away from, 
spots. 
V. The lines C and F vary excessively in thickness over and 
near a spot, and on the 11th in the deeper portion of the spot they 
were much thicker than usual, 
tars in the spectrum of which the absorption lines of hy- 
een are absent, ae either have their chromospheric light radi- 
‘- : 
