864 lY"f. H. H. Turner and Mi. II. K. N-wall. 



after the signal " Start." Mr. Potter, standing by me, received the 

 reading resulting from my observations, and carried it to Professor 

 Turner's hut, and Major Kingsley Foster adjusted the large Savart to 

 the corresponding reading, and the third exposure was begun. 



The camera Savart was left with the pointer at 10 for the rest of 

 totality, no attempt being made to test the permanence in the position 

 of the plane of polarisation of the sky as the total phase of the eclipse 

 passed over. 



Results. The resulting photographs show strong bands over the 

 corona. A cursory examination discloses the following results : 



No. 1. 1 second. Coronal extensions discernible as far as 10' or 11' 

 from the limb. 



No atmospheric bands visible, but obvious bands over the corona. 



No. 2. 5 seconds. Coronal extensions as far as 35' from the 

 limb. 



The planet Mercury appears on the plate. 



Atmospheric bands are visible, very faint, on the following side of 



the sun, extending 4 40' from the limb, but are not visible on 



the preceding side near Mercury. 



No. 3. 20 seconds. Coronal extensions 63' in N/< streamer. 

 52' in S/> streamer. 



70' in N/ streamer. 



Mercury very strong. 



Atmospheric bands visible to the edge of the plate on both sides. 

 Strong bands over^the corona. 



No. 4. 5 seconds. Coronal extensions 35' from the limb. 



No atmospheric bands visible on either side. 

 Nos. 5 and 6. Not examined. 



The existence of the image of Mercury on the plates will l>e of 

 great value in determining orientation in the polariscopic phenomena 

 as well as in the corona. 



The strong bands over the corona indicate that a considerable por- 

 tion of the light is polarised. There are irregularities in the bands 

 which seem likely to afford interesting study just in the way that was 

 anticipated. 



The atmospheric bands faintly visible on the plates are almost certainly 

 due to imperfect adjustment of the Savart to extinction, arising from 

 zero errors, &c. ; they might be due to a change in the position of the 

 plane of polarisation of the sky after the initial setting of the Savart. 

 In any case they are very feeble, and it is clear that it would be well, 

 if ever the experiments are repeated, to dm at imperfect adjustment, 



