The silver state. [volume] (Unionville, Nev.) 1870-1903, 1880-01-14
THE SUNS ECLIPSE.
As Observed by the Members Of the
u. y. Geological sarycy.

Inc BTSb ldHu WHICH Jus SlduOW
touched was the coast of California,
but at such late hour that even there
the sun set partially ecEpsed. The
time of beginning grew later as the
stations were more to the east, till, at a
point near the center of Dakotah Terri
tory, it began at sunset. The fact that
sthe end of the eclipse was not visible
explains why it has been so little
noticed by the astronomers of the East
ern States.
The time of first contact for Eureka
was Oh SIN los P. NJ, local time, 45s
earlier than predicted. This discrep-
ancy is accounted for by the fact that
our longitude has not yet been accu-
rately determined. The moon first
touched the suns disc at point 33aa
degrees to the right of the lowest point,
and passed off at an angle OF 40 degrees
to the suns vertical diameter.
For the purpose of measuring the
amount of an eclipse, astronomers di-
vide the suns diameter into twelve
equal parts called digits; the number of
digits covered by the moon expresses
the extent of observation, Thus, the
extent of Sundays eclipse was 81
digits, little more than three-fourths
of the solar diameter. The time of
greatest observation was at 4:l9, and it
lasted 80 seconds. 1t was at this time
that the above measurement 81 digits,
was taken.
In our previous article on the eclipse
want of space compelled us to omit
mention of several striking features of
total eclipse. These are the corona,
the luminous streamers, and the rose
colored protuberances.
The corona is ring or halo of white
light encircling the sun during the
time of totality 1t is brightest at the
dark limb of the moon, where it has
rosy tint, gradually decreasing in luster
till it becomes indistinguishable from
the faint general illumination of the
sky. For distance Of about 400, 900
miles it appears continuous, then it
radiatcs; its extreme length being
equal to the suns diameter; that is,
$50. 900 miles. These numbers are
from the total eclipses of 1858 and 1850.
The observations of the eclipse of 1873
has established the fact that the corona
is reflected light.
The luminous streamers are also re-
fiected light, and are probably part of
the corona They are broad, separate
bands of light, extending much further
than the corona In the eclipse of
1850 four of these streamers were seen,
symmetrically disposed around the
suns perimeter. They extended to
distance of nearly two million miles.
The rose colored protuberances are
the most beautiful appearances seen
during total solar eclipses. Apparently
they are cloudy masses Of various forms
and sizes just within the dark limb Of
the moon. In some instances they
have been seen entirely detached from
it. They are evidently connected with
the sun, for it has been observed dur
ing totality those in front of the moon
grow shorter, while those behind grow
longer. The prominences have been
seen to extend seventy, and even a
hundred thousand miles from the sun.
The appearance of the sun during
totaity is grand beyond expression.
A large, round, black mass, suspended
in mid heaven, shaded off by beauti-
full rosy tint into the subdued white
light of the corona, and the whole in a
blue background, magni6cently stud
ded with bright stars that have APP
peared as if by magic.
The rosy prominences are supposed
to be burning masses of hydrogen,
elected from the solar surface. Imag-
inc the force necessary to project them