| THE SOLAR SPECTRUM AT THE DATE 1877-1878. 
297 
WAVE- 
NUMBER- 
PLACE of 
single lines, 
and Centres 
of doubles. 
36 862 
36 907 
36 926 
36 936 
36 943 
36 949 
36 954 
36 958 
36 962 
36 968 
36 975 
36 982 
36 984 
36 990 
Differences. 
15 
10 
bo TNO PPO DD 
Telluric lines, 
supposed of 
dry gas. 
Appear- 
lour of th Intensity | @¢¢ bY | wave. 
eeaoncus Object Observed, generally a black, fixed of hack, or eae NUMBER- Diferences 
| Spectrum at Fraunhofer Line. thickness z PLACE of Bates 
the Place. of line. symbol. every line. 
Tenth pair—1st component line, G5) Gill | 36 891 3 
gnd do. do. . co ae 36 894 
: Eleventh line, single, 1:0 | 36 907 
i The above concludes the ‘‘ preliminary’’ band of Great B, and the double lines are eminently sharp, clear, well- 
, defined both within and without, having no haze whatever about them. 
A Next begins the so-called ‘‘ attached” band of Great B. 
; First pair—1st component line, Ors I a 36 924 4 
Qnd do. do. Oe dl. 36 928 
i Second pair—ist component line, 03 |] I 36 934 3 
2nd do. do. 0°5 | 36 937 
BED. Third pair—Ist component line, O38 i, | 36 942 2 
2nd do. do. 0°8 | 36 944 
66 
By Fourth pair, or single line ? 1:0 | 36 949 5 
} Fifth do. do. 2 1:0 | 36 954 i 
} Sixth do. do. 2 0°8 | 36 958 4 
A strong certain single line, 2:0 I 86 962 6 
Another like it, 20 J 36 968 z 
Another rather fainter, 15 | 36 975 
i Great B line, begins with a bundle 
of fine lines—1st edge whereof, 3 ae Hed 
2nd do. : , 
A pale space intervenes, shaded by 
apparently infinitely fine, close 
lines, . c ; : 3 
A strong terminal line, 2 ] 36 990 
du e, is not yet known. All the lines from 36 692 to 36 990 blacken immensely as the Sun goes down. 
The above terminates the whole of the very beautiful arrangement of great B and its bands; supposed to be due to telluric 
‘influence, because it thickens when the sun is low in the sky, but the particular element, or combination of elements to which it is 
' The beauty of the compound and rythmical structure of the lines is much enhanced by the magnificent full and perfect red on 
Which they are depicted when the Sun is high, and no false glare from other parts of the spectrum enters the field of view. 
brightness of the light. 
Appear- ee 
. ance by . ATA, 
! Object Observed, generally a black, fixed eee graphical Re A fro ON 
( Fraunhofer Line. thickness aes a peste eNO 
= Gree symbol. ae mal Solar 
Spectrum. 
| Pil : 
re Suspected fine line, 0°3 ! 
z ‘ De. do. 0°3 1 
be Certain fine line, 1:0 | 37 043 
" Suspected fine line, 0°3 ' 9°765 
Do. do. 0°3 \ 9°782 
q Do. do. 0°3 | 9°834 
= Do. do. 0°3 ' 9-862 
Scarlet- Do. do. 03 1 9°920 
Red. 
Certain fine line, 15 | 10°050 37 195 
Suspected fine line, 0°5 ' 10°160 37 247 
Certain fine line, 1:0 | 10°328 
Suspected fine line, 05 ' 10°426 
Certain very fine line, Jets s 1:0 | 10-913 
Certain fine line, 3 ae 5 16 | 10°992 87 553 
Very fine line, . c é c 2 1) | 11°268 
VOL. XXIX. PART I. 
Chemical-origin- 
data from 
Angstrom, 
Thalen, &e. 
Concluded 
WAVE- 
NUMBER- 
PLACE, per 
British Inch, 
37 013 
37 032 
37 043 
37 084 
37 093 
37 101 
37 122 
37 143 
37 192 
37 242 
37 308 
37 343 
37 526 
37 553 
37 638 
With W.-N. 37 000 the Red of the Continuous Spectrum verges towards a scarlet-red, more or less, partly depending on the 
Differences. 
Breadths & 
Doubles. 
Distances, 
_ 
Ne) 
11 
