OF SPECTRA AT THE SOLAR ECLIPSE OF JANUARY 22, 1898. 
397 
fCr . . 
approximate atomic 
weight 
52 
Mn . . 
• 5 ^ 5 5 
5 
55 
Fe . . 
• 5 5 M 
5 
56 
Ni . . 
• 5 * 5 5 
5 
59 
^ Co ? . . 
• 5 5 5 5 
5 
59 
rSr 
• 5 5 15 
5 5 
88 
Y . . 
• 5 1 '5 
1 5 
89 
L Zr . . 
• 5 5 5 5 
5 5 
91 
Taking the whole series of known elements having atomic weights from 1 to 100, 
ah the metals are here represented excepting the following :— 
Li . 
approximate atomic 
weight 
7 
Be . 
• • 55 55 
• 5 
9 
K . 
• * 15 55 
• 5 
39 
Cn . 
' • 55 51 
5 5 
64 
Zn 
'' 5 ; 
65 
Ga . 
. . . ., 
70 
Ge . 
• • 5 1 > * 
' 5 
72 
Bb . 
• • ' 5 5 
1 5 
85 
Nb . 
• • 5 5 5 ' 
94 
Mo . 
• • * 5 5 5 
96 
Of the nineteen known metalloids, the only ones indicated in these spectra are— 
H . . . approximate atomic weight = 1 
He 
C 
N 
Si ? 
4 
12 
14 
None of the elements with atomic weights exceeding 91 appear to be represented 
in the flash spectrum, unless we Include lanthanum (at. wgt. 138). It is j^robable, 
however, that with instruments of much greater aperture and focal length than the 
one employed in this research photographs would be obtained which would bring to 
light many of the heavier metals which doubtless exist in the lowest strata of the 
flash-spectrum layer. 
Although it would seem from the above statement that there is a general, inverse, 
relation between the atomic weight of an element and the extent of diffusion of its 
vapour abovm the photosphere, it is evident that among the elements actually found 
in the chromosphere this relation does not always hold ; thus calcium and titanium 
ascend to far greater elevations than the three elements of smaller atomic weight, 
sodium, magnesium and aluminium. 
Unknown Lines .—Only a small })ro})ortlon of the lines in Table 1. remain to he 
