362 Rev. A. L Cortie [Feb. 26, 



it suggests the genesis of the " maximum " type, as the superposition 

 of bright streamers on the two long wings in the equatorial regions, 

 which probably are a sub-permanent feature of all coronte. The 

 N.E. streamer is projected over the background of the continuous 

 corona, and consists of a sheaf or bundle of very bright rays, which 

 can be traced as far as 26' from the sun's limb. The filamentous 

 nature of the other streamers is also marked. The lower corona is 

 represented by a bright continuous ring all round the sun, l)etween 

 1' and 2' of arc in depth. This is seen on both the large scale and 

 small scale photographs. A considerable arc of the chromosphere is 

 shown on the W. limb, on the last-exposed of the larger scale photo- 

 graphs, as the slide was only just closed before the end of totality. 

 The southern boundary of the S.E. streamer extends farther from the 

 sun than any other feature, fully two diameters. It has a marked 

 double curvature. On the ^\. side of the corona at position angle 

 356°, inclose proximity to a small bright prominence, is a remarkably 

 distinct filament, which can be traced as far as 7' from the sun. It 

 curves over towards the equator. Immediately below the filament 

 are the bright edges of two shorter streamers, which are superposed 

 upon the main mass of the coronal wing. These three bright rays 

 are as characteristic of the N.W. limb as the bright sheaf of rays of 

 the N.E. limb. AVe shall discuss their probable import in a sub- 

 sequent part of this discourse. 



The spectrum of the corona next claims our attention. Although 

 extremely weak on the plate it is quite measurable. The corona was 

 a bright one, yet the well-known green radiation of the coronal light 

 about wave-length 5303 is inconspicuous, though just discernible on 

 the plate. This result agrees with that obtained by other observers. 

 Secondly, the intenser radiations are in the red end of the spectrum. 

 Other observers of the eclipse have called attention to a well-defined 

 bright radiation about wave-length 6374. This line is one of the 

 strongest on our negative, but it is not an isolated radiation. It 

 occurs as a member of one of a series of three bands or flutings at this 

 end of the spectrum. The wave-lengths of these terminal lines areas 

 follows : — 



, (6643-9) m r o ^6530-91 q. y 



1- ■(6630-5) T^^^'^^^"^^^- 2- i6502-8] ^^^^^"^'• 



^- |6363-*0|^^^^^li^^^- 

 Two other bands occur at wave-lengths — 



, (5118-1) rr V . (5315-3) ^^ y 



*• 15114-3) T^^l"^^^- ^' 15302 • 7f ^^'^^*^"^'^- 



All the lines in these bands are sharp, though the images are very 

 faint. There are also other lines visible which have not as yet had 

 definite wave-lengths assigned to them. The general character of the 



