the solar photosphere, This has been partially cleared up, and as far as our 

 present knowledge warrants us in stating the matter, the solar envelopes are as 

 follows : — 



The Photosphere and Chromosphere (the latter term will probably be before 

 long abolished) form the denser portion of solar atmosphere. This was estab- 

 lished previous to the late eel pse. The former is the portion ordinarily visible 

 to the eye in the telescope, is in fact the visible limb of the sun ; the latter is 

 visible only in the spectroscope, except during total eclipses, the one being a 

 continuation of the other, and differing from it, if difference it may be called, 

 merely in the diminished pressure of the component gases. 



Beyond this we come to a bright, pearly, and very irregular ring, forming 

 the inner portion of the corona, and having to the eye a different character from 

 it. The piotuberant irregularities of this ring closely correspond to the red 

 flames or protuberances, which we are all familiar with, and which are now 

 ascertained to be eruptions of glowing gases, principally hydrogen. This envelope 

 seems to be of pretty uniform density or brightness, and does not fade away very 

 much as its distance from the sun increases. It has been proposed to call it the 

 " Leucosp'aere," or white envelope, but these terms are not likely to hold their 

 place very long, and may be considered as only provis onal. 



The probability is that this "white envelope" forms, with the positions im- 

 mediately below it, a distinct part of the solar atmosphere, wh-ch seems to be 

 characterised chiefly by the gradually decreasing pressure of the component 

 gases; though in what particulars this atmosphere differs from the outer radial 

 portion hitherto popularly known as the corona proper, it is impossible yet to say. 

 Beyond this white envelope we find an extensive glow with a marked radial 

 appeirance, which has somewhat of a violet colour, tinged with faint rose and 

 green, according to some observers, and gradually fades away, as it recedes from 

 the sun, until it at last takes the form of rays, disappearing in a faint glow. 

 On some occasions these rajs have been veiy marked, as they were during the 

 late eclipse, and commenced a"- no great distance from the sun's limb. 



As totality approached on December 22nd, when the denser portions of 

 the sun's atmosphere were eclipsed, the continuous dark band spectrum gradually 

 disappeared, the telescope remaining pointed always to the same spot, and three 

 bright lines C D and F made their appearance, which was identified by means of 

 the vacuum tube. In a few seconds more C and D disappeared and two sharp 

 bright lines were seen. One of these is coincident with the bright hydrogen 

 line F ; the other is on the less refrangible side of b, and is considered to be a 

 new element. The distance of the spot observed, in this instance, from the sun's 

 limb appears to have been about 7 1 or 8\ 



But here a difficulty arose. Owing to our atmosphere being itself illumi- 

 nated by this peculiar light it was of course impossible to ascertain its limits, i.e., 

 how far into the corona these bright lines really extended. Now it is worthy of 

 remark, as being probably a point of great importance, that this new bright line 



