OF SPECTRA AT THE SOLAR ECLIPSE OF JANUARY 22, 1898. 
391 
East limb . 
West limb 
Position angle of 
maximum intensity. 
I 57° to 78° 
1 94 „ 100 
235 „ 254 
As in No. 6 spectrum there is an exceedingly faint impression of a corona line 
near H and extending over the west limb, but excepting this no trace of any other 
lines are visible. The image, unfortunately, is too feeble in the extreme idtra-violet 
to show the line at X 3388 found on No. 5 spectrum. 
Spectrum No. 8.—This negative was exposed for about half a second almost at the 
moment of third contact. The reappearing photosphere has been impressed as four 
very narrow streaks of continuous spectrum. The Hash spectrum is well developed, 
and the whole length of the spectrum is crowded with bright lines extending 
between and across the strips of continuous spectrum. The majority of the lines due 
to the lower chromosphere extend over an arc of 55°, the depth implied in this case 
heing 2'''5. 
The focus in this negative is unfortunately very poor throughout the spectrum, 
and no measurements were made for determining wave-lengths. The spectrum was, 
however, carefully compared with No. 3 by means of enlargements of each spectrum, 
which were made to corres})ond approximately in scale. Superposing one spectrum 
upon the other it was found that the two appeared to be identical in all respects. If 
any differences exist at all between the spectra of the east and west lindjs of the sun 
they can only be found in the finer details, which in No. 8 are lost l)y reason of the 
imperfect focus.'*' 
'The Cusp Spectra after 'Totality. 
Specto'a Nos. 9 a7id 10 (Plate 10, fig. 3).—These were given an ex})osure of less 
than half a second at about 10 and 18 seconds after third contact respectively. They 
are both very similar to the first two spectra of the series, but apparently the 
exposures were appreciably of longer duration than those made before totality, and 
the bright lines bordering the continuous spectrum of the photosphere are in conse¬ 
quence much more strongly marked than in Nos. 1 and 2. 
As in all the spectra of the west limb the focus is imperfect except in the ultra¬ 
violet regi<m more refrangilde than X 360. The briglit lines are, however, fairly well 
dehned along the south edge of the cusp. 
The Fraunhofer spectrum is not nearly so well developed in these spectra as it is in 
Nos. 1 and 2. Tliis may be due to over-ex})osure as well as })oor focus, but at the 
ultra-violet end where the spectrum is less dense and the focus good, tlie dark lines, 
* No figure is given of this photograph as it was found impossible to produce a satisfactory jjlate 
suitable for reproduction. 
