156* Postscript 



state that in their spectroscopic observations, the ordinary spec- 

 trum of the chromosphere and hydrogen flames was seen, and 

 outside of the part of the spectrum due to the chromosphere, there 

 was a clear green line. As to the nature of the green line they 

 have only the fact that the lines were not those of hydrogen, or of 

 iron, or of any known terrestrial substance. 



It is further stated that the corona, according to an observer 



retiected light ; and it is polarized in such a way as to prove that 

 it is not atmospheric ; and hence, it is added, it may be considered 

 as a solar appendage reflecting in an eclipse the light of the ob- 

 scured sun. Prof. Watson asserts that he has seen a part of the 

 corona float away " like a vail," which suggests that its matter is 

 constantly dispersing. 



Observations of Prof. C. A. Young, Jerez, Spain, (Tribune, 

 Jan. 25th). — The sun was obscured until totality, and just then a 

 small rift in the heavy clouds opened the sun to view, and gave an 

 opportunity for excellent observations. One good photograph of 

 the corona was obtained. Prof Young writes as follows : 



Om- spectroscopic results completely coniirm those of last year, 

 except that the two faint lines, which 1 saw between U and E last 

 year and suspected to be corona lines as well as 1474, were not 

 seen at all this time ; 1474 was traced by Prof. Winlock to a dis- 

 tance of nearly 20' from the sun's limb. I traced it 16' on the 

 West, 12' on the North, 14' on the East, and about 10' on the 

 South. The principal chromosphere lines were also visible in the 

 corona to a distance of 3' or 4'. Prof. Winlock and myself both 

 agree in attributing this to the reflection of the haze around the 

 sun. I am more confident as to this, because last year, in a clear 

 atmosphere, the C line was certainly sharply terminated at the up- 

 per limit of the chromosphere or prominences under observation, 

 le most interesting spectroscopic observation of the eclipse 

 to me to be the ascertaining at the base of the chromo- 

 nd, of course, in immediate contact with the photosphere, 

 a layer in whose spectrum the dark lines of the ordinary 

 solar spectrum are all reversed. Just previous to totality, 1 had 

 carefully adjusted the slit tangential to the sun's limb at the point 

 where the second contact would take place, and was watching the 

 gradual brightening of 1474 and the magnesium lines. As the 

 crescent grew narrower, I noticed a fading out, so to speak, of aU 

 the dark hues in the field of view, but was not at all prepared for the 

 beautiful phenomenon which presented itself when the moon fin- 

 ally covered the whole photosphere. Then the whole field was 

 at once filled with brilliant lines, which suddenly flashed into 

 brightness and then gradually faded away until, in less than two 

 seconds, nothing remained but the lines I had been watching. 

 The sUt was very close, and the definition perfect. , . , 



Of course I cannot positively assert that all the bright lines held 

 exactly the same position that had been occupied by dark ones 

 previously, but I feel very sure of it, as I particularly noticed sev- 

 eral groups, and the whole arrangement and relative intensity 

 struck me as perfectly familiar. 



This observation is a confirmation of Seech i's continuous spec- 

 truui at the edge of the sun, and I think tends to make tenable tbe 

 original theory of Kirchoff" as to the constitution of the sun and 

 the origm of the dark lines in the ordinary solar spectrum. 



appears 



