OF SPECTRA AT THE SOLAR ECLIPSE OF JANUARY 2?, 1898. 
411 
Table II .—Spectrum of Prominence. 
The wave-lengths given in the first column of this table are deduced from measures 
of the images of a very small bright prominence in spectrum No. 4, This prominence 
was situated almost at the point of second contact at position angle 59° (solar 
latitude -T 23°). 
The photograph was exposed at the beginning of totality immediately after the 
disappearance of the flash spectrum. 
The prominence images are well defined circular spots in all radiations except the 
calcium and brighter hydrogen rays, which show wings due to motion in the line of 
sight. 
The columns of this table are arranged as in Table I., and the intensities in 
column 2 were estimated in the same way as those of No. 3 spectrum given in Table I. 
The helium wave-lengths given within brackets in column 4 are from IIunge and 
Paschen. 
Table II. 
tVaveJength 
No. 4 
Remarks. 
Wave-length, 
solar 
*«2 
4-i 
$ 
spectrum. 
-4^ 
spectrum. 
Rowland. 
44) 
hH 
0 
s 
3435 
Limit to -p/hich continuous spectrum of pro- 
minence can be traced 
3534 r 
Continuous spectrum is much brighter at 
3535-554 
4 
Ti 
3537 \ 
this point 
3614-0 
0 
3613-947 
4 
Sc 
3618-9 
0 
3618-919 
20 
Fe 
3625-3 
0 
One measure only. 
5 
Ti 
3631-6 
1 
15 
Fe 
3634-6 
1 
(3634-393) 
— 
He 
3668 ± 
— 
Beginning of continuous spectrum in promi- 
—- 
— 
— 
nences 
3669-52 
^ 1 
— 
-- 
llxp 
3671-61 
0 
1 
Rarther difficult to measure. 
— 
— 
Hx 
3673-92 
0 
f 
vSilver deposit very -iveak. 
— 
— 
H</. 
3676-55 
0 . 
— 
— 
Ha 
3679-55 
1 ] 
— 
— 
Hr 
3683-06 
1 
— 
— 
Her 
3685 - 34 
3 
3685 - . 3.39 
10 
Ti 
3687-12 
1 
— 
— 
lip 
.3691-75 
1 
_ 
— 
H- 
3697-18 
1 
_ 
— 
Ho 
3704-11 
1 
__ 
— 
Ht- 
3705-86 
1 
■ 
Well-defined and very small circular dots . 
3705 - 708 
9 
Fe 
3712-19 
2 
. .. . 
— 
Hr 
3720-02 
1 
.3720-084 
40 
Fe 
3722-07 
2 
_ 
— 
H/x 
.37.34-52 
2 
_ 
— 
HA 
37.37-27 
1 
30 
Fe 
.3741-79 
1 
. 
.... 
13741-205 
4 
4 
Ti 
Ti 
3 (i 2 
