410 
SIR NORMAN LOCKYER AND OTHERS 
paratively faint. The small prominence No. 10 and the long thin one No. 3 appear 
in H and K and the lower part of the latter is shown feebly in and Hy, Those 
richest in bright lines are numbers 5 and 8, the spectra of which are indicated by 
the following table. The wave-lengths and probable origins are taken from the 
table of chromospheric lines which forms part of my report on the eclipse of 1898. 
In the column of origins the prefix ‘p is an abbreviation for proto, indicating that an 
enhanced line in the spectrum of the substance in question agrees in position with 
the prominence line, enhanced lines being those which are intensified in passing from 
the arc to the spark spectrum. 
Spectrum of Prominences Nos. 5 and 8. 
Wave-length. 
Photographic 
Intensity. 
I 
Probable Origin. ; 
Remarks. 
3685-34 
1 
pTi 
3711-9 
<1 
H 
Hr 
3721-8 
1 
H 
Hp 
3734-15 
1 
H 
HA 
3750-2 
2 
H 
H/c 
3759-45 
3 
p Ti 
3761-46 
3 
p Ti 
3770-7 
2 
H 
Ht 
3798-0 
3 
H 
He^ 
3820-59 
1 
Fe 
3835 - 6 
5 
H 
Hr; 
3860-06 
1 
Fe 
3889-15 
8 
H 
3900-68 
1 
p Ti 
3913-61 
1 
pi:i 
3933 - 83 
10 
p Ca 
K 
3968-63 
10 
p Ca 
H 
4026-34 
4-5 
He 
4045 - 98 
<1 
Fe 
4077-89 
4 
Sr 
4102-00 
8 
H 
m {h) 
4120-97 
<1 
He 
4215-70 
3 
Sr 
4226-90 
<1 
Ca 
4247-00 
< 1 
Sc 
4340-63 
8 
H 
Hy (G) 
4395-20 
<1 
p Ti 
4471-65 
5 
He 
4687-0 
<1 
_ 
4713-25 
1 
He 
4861-53 
8 
H 
H/3 (F) 
4922-10 
<1 
Ast 
5015-73 
<1 
Aet 
5183-79 
1 
Mg 
In 
5875-87 
6 
He 
D. 
6563-05 
2 
H 
1 
Ha (C) 
1 
A comparison with the chromospheric arcs indicates that the spectrum of the 
