Catoctin clarion. [volume] (Mechanicstown, Md.) 1871-1940, 1900-05-03


there must be a total eclipse of the sun al all
places within this shadow. If, however, at
the time of the eclipse the sun is nearest to
US and the moon hrthest. the moons disc
appears smaller than the suns, and 1t doesn t
hide it all, In this case the moons shadow
does not reach the surface Of the earth, and
ring of tight will be seen around the edge
of the sun, giving rise to an annular eclipse,
so called from Latin word meaning ring"
Under the most favorable circumstances the
breadth of the cross-section Of the moons
shadow is 1877 miles the largest value posi-
Bile. BY the interposition of the moon be.
tween the sun and the earth also kind of
halfshadow, technically called penumbra, Is
produced, the greatest cross section of which
on the earth is 4,500 miles in diameter. An
observer situated within this penumbra OBJ.
serves a partial eclipse. If he Ia near the
shadow cone, the sun will be mostly covered
by the moon, but if near the exterior limit OF
the penumtrs, the moon will only slightly
encroach on the suns disc. While total
eclipse is visible as such only by an observer
within the narrow path traversed by the
shadow, the same eclipse Is visible as partial
by everyone one within about two thousand
miles on either side of the shadow path. In
a lunar eclipse the moon overtakes the shad
ow of the earth and consequently her eastern
limb enters the shadow first, 80 that lunar
eclipse always begins on the east side of the
moon and ends on the west side. In Il solar
eclipse, however, the moon in her eastward
motion overtakes the sun and conceals the
western limb first, so that solar eclipse be-
gins on the west side of the sun and ends on
the east side. The path of the total eclipse
occurring on the 28th Of the month will pass
through the northern part Of Mexico, through
the cities of New Orleans, Mobile, Raleigh
and Norfolk in the United States, across the
Atlantic Ocean between the fortieth and
flftieth parallels of latitude, traverse Spain
almost in the middle Of the peninsula and the
Barbary States OF Africa, notably the city OF
Algiers. AS to the United States, Norfolk,
Va, may be regarded as the most northern
point through which the shadow cone of the
moon will pass AS regards impressivcness
and sublimity, nature, so lavish in presenting
beautiful spectacles Of the most varied kinds,
exhibits no finer phenomenon than a total
eclipse of the sun. The suns outer atmos
phere-the corona-wbich is never seen ex.
cept during total eclipse of the sun, app cars
as a bright cioud.lke circle Of light sur.
rounding the darkened sun. The suns low
er atmosphere-the chromosphere-tha lay.
er of burning gases which thousands of
during a total eclipse of the sun, projecting
tongues Of flames, which indicate what ter
ribe storms are continually raging in the
solar atmosphere. 1t cannot astonish us
chat in ancient times and during the dark
ages solar eclipscs were always looked at
with sensations Of fear and awe, when we
consider that experienced and professional
observers are themselves unable to suppress
feeling of awe during this wondrous spectacle
of nature. When that tremendous shadow
cone approaches with velocity that makes
us recoil with an involuntary shudder, as
though it would cngulf us forever in it awful
darkness, even the otherwise unfuiling in
stlnct of the animal creation is deceived.
Wild beasts, atfrighted, hasten to their lairs.
birds futter uneasiy in the air and seek
their nests, cattle anxiously begin to low, all
animals, their instinct failing them, are aSi-
tated. The countcnances OF the spectators
assume ghastly, cadayerous palor, and the
the light, as much as there is, has wcrd
lurldness which lntensifies the appalling
character of the spectacle.
Observations made during total solar
eclipses are OF such Importance as to induce
the governments Of different countries to
send out professional astronomers for this
purpose. We briefly mention few of these
important observations that arc made and
can only be made on that occasion. By &C.
curately observing the times of the four con.
facts the relative position ofthe sun and moon
can be determined and the tables Of their
motion corrected. Intramcrcurial planets
can be searched, Photomcric measurement
can be made of the intensity of the light at
different stages of the eclipse and during to
tality; also spec,roscop,c observations upon
the spectra of the lower atmosphere of the
sun, the prominenccs, and the corona. Pho
Biography will play an important part and
will bring forth important results
Here about nine .tenths Of the sun will be
obscured at the middle of the eclipse, but
that one,tenth of bright surface will rob us
Of all the magnlfcence of a total eclipse and
there will be nothing particularly striking
other than a perccptible dimunition of the
light Of day.