TOTAL ECLIPSE OF THE SUN, JANUARY 22, 1898. 
207 
(l.) The coronal rings may be divided into three groups, defined by the position 
angles in which they have their greatest brightness. The typical rings are at wave¬ 
lengths 5303'7, 3987, and 4359'5. 
(2.) The different forms of the coronal rings indicate that they are not all due to 
the same substance, at least three being in question. 
(3.) The origins of the rings have not yet been traced. 
(4.) There are possibly feeble indications of some of the chromospheric gases in the 
inner corona. 
(5.) The chief coronal ring in the green is very closely associated with the form of 
the inner, and appears to have no distinct connection with the outer corona 
(6.) The outer corona gives no indications of bright lings in photographs taken 
with the prismatic cameras. 
Further examination of the photographs has shown that some of the most minute 
detail of the inner corona is represented in the green ring. Near the equatoi', on tlie 
eastern limb, for instance, there is a well-defined loop-shaped structure in the innei- 
corona, which presents almost the appearance of a prominence, and this is faithfully 
reproduced in the corresponding part of the green ring ; its spectrum, however, has 
nothing in common with that of the prominences. A similar relationship is shown at 
other position angles, but as the Viziadrug photographs were all exposed too long to 
clearly separate the inner from the outer corona in all parts, a complete discussion of 
this point must be deferred until photographs taken with shorter exposures by other 
observers become available for comparison. 
The table of coronal radiations is reproduced at the end of this report in order to 
facilitate comparisons with the chromospheric radiations. 
The Continuous Spectrum. 
The coronal rings are superposed upon a continuous spectrum which is broken up 
into bands of various intensities (see Plate 7), and it is importanf to note that each 
bright part of the green ring is accompanied by one of these bands. In some of the 
photographs a few bands of continuous spectrum are seen apparently without 
corresponding brightenings of the green ring, but an examination of the other 
photographs generally reveals the brightening in a lower reach of the corona. One 
or two of the bands appear in places wdiich correspond to The points on the sun’s 
limb about 90° degrees from the points of second and third contact, and in these cases 
the corresponding brightenings of the green ring are probably hidden by the moon 
throughout the eclipse. 
These facts indicate that the action w^hich produces a brightening of the green ring 
also produces a brightening of the continuous spectrum, not only in the region where 
the gaseous mass is rendered more luminous, but in the region immediately overlying 
it. The continuous spectrum of the outer corona exhibits no definite structures in 
