Screntifie Intelligence. 245 
no mistake, as C was even more brilliantly eg arg at the 
same time. What the substance which causes it may be is quite 
unknown. Like the so-called D, line it has no corresponding dark 
i tru 
m. 
e same observer, and the writer also, saw both H lines (cal- 
cium) brightly reversed in the spectrum of the chromosphere ; 
thus confirming observations made six years ago at Sherman, but 
never corroborated since, except by the ilcieagrigisia spectrum 
obtained by the Siam expedition in 1875. 
he exquisite reversal of the ~ Fraunhofer lines at the mo- 
ment of totality w b of the observers. Several 
the principal dark Fraunhofer lines in the corona spectrum, thus 
showing that a considerable percentage of the —— radiance is 
mere reflected sunlight. The dark lines were, however, so faint as 
to be seen by very fe ‘few and this shows equally ety we think, 
ve 
Wright, gomatcy Harkness and others—are emphatic and iene 
in their contrary conclus 
Experiments with ae seas or new heat measure of Mr. 
Edison showed, as was ascertained m ears ago, that the heat 
of the corona is quite sensible. With ¢ a " rmopile attached to a 
acces peer wns ty Mr. Anderson, of the Princeton 
oub 
t hes been represented i in some quarters that the rome of this 
eclipse require a fundamental reconstruction of the es hith- 
erto held regarding the enaiadintice of the corona. This is, how- 
ever, an entire misapprehension. The same calcein: spe 
in the corona as hitherto, only in altered proportions, as might 
have been and was - by students of solar physics. In 
1869, 1870 and 1871 the gaseous elements of the corona—the 
hydrogen and “1474 stuff ” whatever that may be—were in such 
quantity and condition and rose so so high above the solar surface 
that their lines were conspicuous in the coron 2 erties 
attracted the attention of observers far more forcibly than the 
feeble continuous spectrum of the light emitted from and reflected 
by, the minute solid or liquid particles which also constitute an 
essential element of the corona. At present the condition is re- 
: gases are either too small in quantity or too cool to 
be conspicuous. The | esson, and it is an important one, is simply, 
