ON THE TOTAL SOLAR ECLIPSE OP MAY 17, 1882. 
265 
An instantaneous photograph taken in the prismatic camera about 5 seconds 
after the end of totality presents one or two peculiarities which are worth noticing. 
In the first place, the prominences still appear, except at the places at which 
their light is overpowered by that of the sun. The continuous spectrum of the sun 
is broken up into three or four parallel bands—an appearance no doubt due to the 
irregularities on the moon’s surface. We have here Bailey’s beads drawn out into 
bands. At the solar cusps traces of rings are seen which are due to the lower parts 
of the chromosphere extending beyond the cusps. The two brightest of these rings 
correspond apparently to the solar lines F and G. 
We give in conclusion a table showing the lines which are seen in different 
prominences. The numbers indicate the order of intensity for the same line in 
different prominences. Thus, for instance, it is seen that in I., C is fainter than in the 
prominence 11.; while the order is reversed for the line F. 
Relative intensities of lines in the prominences. 
Prominence = 
I. 
n. 
III. 
IV. 
V. 
71 1 
Below \ 10,000 
Faint 
8240 (?) 
Distinct 
Probably a 
hydrogen line. 
6562 (C) 
3 
2 
1 
5875 (D 3 ) 
5315 (1474*) . . 
3 
Very faint - 
2 
1 
4861 (F) 
2 
1 
O 
O 
V ery weak 
5 
4 
4471 (f) 
3 
2 
l 
4394 .. 
l 
4340 (H 7 ) .. 
3 
2 
1 
Weak, but 
stronger tlian F 
4 
5 
4101 (h) 
3 
2 
1 
4 
3968 (H) 
3 
2 
l 
3933 (K) 
3 
2 
1 
5 
4 
Many lines in ultra- 
violet 
Results of the spectroscopic camera. 
The slit of the spectroscope had a direction approximately north and south, but it 
did not accurately pass through the centre of the solar disc, and we have no data to 
fix accurately on the regions of the corona through which it passed, although its 
approximate intersection of the image can be guessed, as will be seen further on. 
The photograph shows, in the first place, a strong continuous spectrum. This is 
neither equally strong nor equally extended on both sides of the moon’s disc. On the 
northern side the spectrum can be traced to a wave-length of about 3490 towards the 
ultra-violet; but on the southern side it reaches further and almost as far as the solar 
MDCCCLXXXIV. 
* Kirchhoff’s scale. 
2 M 
