l'l-Itf SCU ANTON TRIBUNE-SATURDAY, MAY 2G, IWO.
OJJ
THE SUN WILL BE
IN TOTAL ECLIPSE
NOTABLE ASTRONOMIC EVENT
EXPEOTEDON MONDAY.
An Export Analysis of tho Physi
cal Constitution of tho Sun, and
Somo of tho Things Astronomers
Expoct to Establish During tho
Totality of May 28.
From Ihf PlttiburR- I)ipatch.
A total eclipse of the sun Is one of the
most Interesting phenomena ot nature,
but occurrlnc as It usually docs over
widely-separated parts of the earth,
and over a comparatively marrow belt
of land, It Is by any one person wit
nessed but seldom, even by professional
nstronomers.
On May 28 there will be a total
eclipse of the sun visible In the south
eastern part of the United States. Its
path, the track of the moon's shadow,
within which alone the Interesting
phenomena of the eclipse are visible,
covers a belt about CO miles wide, the
center of which stretches In a nearly
straight line between a point a little
south of Norfolk, Va and another a
little north of iNew Orleans. The time
during which tho sun Is totally
eclipsed Is short, being 72 seconds on
tho line of centrallty near Now Orleans
and 100 seconds near Norfolk.
However, brief as Is thj Interval of
totality on this occasion, It does not
even under the most tavorable cir
cumstances quite equal eight minutes.
But so valuable Is the knowledge to be
gained during tho few seconds of a
total eclipse, ni to be obtii nod, be It
said, at no other occasion, that oven
at the risk of clouds robblnff him of
the fruits of his labor, the astronomer
Is fully Justified In tho great expense
of time and money connected with a
distant voyage to observe a total
eclipse of the sun.
A STUDY OP THE SUN.
To understand In a measure tlu
scientific Importance of a total eclipse
the problems It may solve some idta
of what modern research has revealed
concerning the nature of the sun Is
necessary.
The Importance of the sun to the
life of man has been recognized, even
at the dawn of civilization, when he
worshipped It as a god, as Indeed some
savage tribes do still. However, few
are awaro cf our absolute dependence
upon Its light and heat. Not only
does every form of life depend directly
on the sun, but all forms of energy,
except contact electricity, that part of
the tidal wave duo to the attraction
of the moon, and the Interior heat of
the earth, have their origin in the
sun's rays.
It Is the heat of the sun that moves
the vast mechanism of the earth'3
ntmosphore, that evaporates the enor
mous quantity of water which de
scends In the form of rain or snow,
and the energy of Its rays that enables
plant life to absorb the carbon from
tho carbolic acid gas In the air and
build It into Its tissue, while the purl
fled oxygen Is restored to the atmos
phere How great the work done by
circulating the water through the at
mosphere will appear when we consid
er that If nil the water annually evap
orated at the equator were collected
in a basin the size of the United States
it would fill It to a depth of about 200
feet. Of the power which this would
yield In again descending to the sea,
tha 2,000,000 horse-power, which it is
estimated the Niagara Falls would
yield, Is but a very small fraction.
ESSENTIALITY OF SUN-HAYS.
How Important the chemical action
of the sun's rays is, not only to plant
life, but also In purifying the atmos
phere, Is seen from tho estimate that
the breath of man adds annually to
the atmosphere five and one-half bil
lion tons of carbonic acid gas, which
if permitted to accumulate, wouli
double the normal amount In the air In
about COO years, and render tho pro
cess of breathng exceedingly difficult.
Even the heat obtained from coal
which we use to warm our homes and
drive our engines comes originally
from the sun, for coal is known to bo
of vegetable origin. Thus In burning
coal we are using the energy of sun
light stored up long befora the adve.it
of man.
These facts, though interesting, fur
nish no accurate value of tho light and
heat received from the sun. For the
purposes of science definite measure
ments must be made. The quantity of
light and heat which falls on a given
area of the earth when the sun Is di
rectly overhead must bo deUrmlned.
Actual measurements show that when
the sun Is overhead on a clear day
It will light up a sheet of white paper
ns brightly as 288,000 standard candles
at a distance of 40 Inches. A 10,000-
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candle power arc lamp In one of the
brightest lights generally produced,
but It must bo brought to within
eight Inches to Illuminate a sheet of
white paper tin brightly ns tho sun
Bond found that sunlight is 470,000
times ur bright as the light of tho full
moon.
NOT ALL HAYS VISIBLE.
By measuring the hent of the sun
the energy, of all Its rays Is determined
that of the dark heat rays as woll
as of the visible rays. There Is no
real difference In the natur" of the
visible rays we call light, or.d those
which can be detected merely by their
heating effect or by means of photo
graphy. The difference Hen In our
sense organs, which respond to some
rays more readily than to others.
One of the simplest wnyn lor de-
tcnnlnatlng the hent effect of tna sun
Is to expose to Its rays n hollow cop
per disk covered on the side oward the
sun with lampblack, so ks to absorb
all the heat, and filled with water In
which Is Immersed a delicate ther
mometer. The rise In tho tompr-ratur
of the water after exposing the dink
for a given time is measured, and this
with the weight of tho water healed,
enables one to measure the quantity
of heat. By such means It Is found
that Mie heat annually ri"'elvej by
the enrth would melt a layer of ice
134 feet deep all over its surface. It
the sunlight were equally dlstilbuttd
In all latitudes; or using the known
relation between heat and worK, the
heat received by each square yard
when the sun is oveihead Is equal to
about one and one-fourth horse-power
of which about one-eight iu mechani
cally available by the use of machines
such ns those constructed bv Erleks
son and Mondrot. It Is found, how
ewr, that the coat of the murhlnu for
the power obtained makes it c( m
mcrclally impracticable.
MEASURING THE SUNLIGHT.
Wo live, however, at the bottom of
a sea of air through which th,e sun
light must penetrate to the earth. II . v
much of the sunlight which falls on the
upper regions of tho atmosphere pene
trates to Its depths? To make such
measurements we cannot pass above
tho atmosphere, but wo can ascend
some high mountain, and, leaving half
tho mass of the air below, measure
the sun's light and heat, and then de
termine the total effect of atmospheric
absorption by computation.
A few years ago the director of the
Allegheny observatory, Professor S. I.
Langley, organized an expedition to
Mount Whitney, Cal , for the purpose of
making such measurements. Mount
Whitney, which Is 15,000 feet above
tho level of the sa, rises abruptly from
a desert plane, in an atmosphere pe
culiarly dry and clear. By making
measurements at the foot of the moun
tain and on its heights the absorptive
power of the atmosphere could be
determined. Professor Langley found
that tho atmonshere has a sifting ac
tion on sunlight, absorbing more of
tho blue and violet rays than of tho
red, so that should the air be removed
the sun would appear blue.
It was also found that tho atmos
phere permits only half of the sun's
heat to penetrate to the surface of the
earth, while at the same time It acts
as a blanket to prevent the heat from
being Immediately radiated into space.
On the mountain top the members
of the expedition, when not exposed to
the direct rays of the sun, suffered con
siderably from cold, but in the sun's
light they suffered still more from Its
burning and blistering rays. Professor
Langley estimated that, If tho at
mosphere were removed, the tempera
ture oven at noon would be far below
freezing.
Having thus found that the heat
which reaches tho upper regions of
the atmosphere Is about 40 per cent,
more than that which penetrates the
surface of the earth, or about l3i
horse power for every square yard, It
can be calculated how much heat Is
radiated at the surface of tho sun,
DIMENSIONS OF OLD SOL.
Now we know that the sun Is a globo
S6C.500 miles In diameter, having a sur
face 12,000 times and a. volume 1.S00,
000 times ns great as the earth. The
earth might be placed at the center of
the sun, the moon still revolve nbout
It as now nt a mean distance of 239,000
miles nnd be but little moro than halt
way toward the solar surface. About
the sun tho earth revolves In a nearly
circular orbit, nt a mean distance of
93,000,000. Imagine a sphere of this
radius surrounding the sun. The earth
will, of course, bo on the surface of
this sphere. We know the heat which
falls on each square foot of the earth,
when tho sun is directly overhead, con
sequently wo know how much heat
falls on our Imaginary sphere.
Now suppose this sphere (shrinks un
til It touches the sun; there now falls
on Its surface the same total amount
of heat as before, but each square foot
receives moro heat, as much more as
the area of the sphero with the earth's
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Fre TsrSsaS Tpostimont
distance from the sun for Its radius
exceeds tho area of the sun Itself.
This brings us to figures which stag
ger the Imagination. It Is found, to
quote the language of Professor Young,
that "this hent radiation at the sur
face of tho sun amounts to over 100,
000 horso power per square meter con
tinually acting; that If the sun were
frozen over completely to a depth of
EO feet, tho heat emitted Is sufficient
to melt this whole shell In one minute
of time; nnd that if nn Ice bridge
could bo formed from the earth to the
sun by n column of Ico 2 1-4 miles
square at the base nnd extending
across the whole 93,000,000 of miles
and If by some means tho whole of the
solar radiation could bo concentrated
uoon this column, It would be melted
In one second of time, nnd between
seven and eight seconds more would
be dissipated In vapor."
TEMPERATURE OF THE SUN'S
SURFACE.
What must be tho temperature of
such a body This question can be
answered, If the law connecting the
quantity of heat radiated by a body
and Its temperature be known. Tl.e
answer, however, can only be given
for the surface of the sun, not for
Its Interior, nnd even then the ojsutnn
Hon must be made that the sun ra
diates like an absolutely black body.
The values found according to the law
of radiation assumed ranged all the
way from 1,500 degrees to 10.000,00)
degrees. The former Is evidently too
low, the latter very much too high.
Professot Langley first made deimlti
measurements to set a lover limit to
the sun's temperature. He compared
tho surface of the sun with tho mol
ten steel In a Bessemer converter, and
found that lio brilliant stream of
whlto hot liquid steel poured from a
Bessemer converter appeared l'ke
black coffee In comparison with th
sun, and that the solar surface ra
diated 87 times as much heat and 5,o00
times as much light as an equal sur
face of the molten steel.
The burning glass frunishes another
means for setting n lower limit to the
sun's tcmeprature. It Is known from
theory that the burning glass cannot
form an Image hotter than the sun
Itself. The effect Is as though the sun
were brought nearer the earth. With
such a glass 40 inches in diameter,
which made the Image of tho sun as
hot as Its rays would bo were It
brought ns near to the earth as the
moon, Ceraskl succeeded In not only
melting, but reducing t vapor all
available tcrrcstial substances.
If, then, the earth should approach
the sun ns clohe as the moon is to tho
earth, It , would not only be melted,
but largely reduced to vapor. Recent
experiments have shown that the ra
diation increases as tho fourth power
of tho temperature. This law gives
the temperature of the sun, allow
once being made for the absorption
by the solar atmosphere, at 8,000 de
grees. PHYSICAL CONSTITUTION OF THE
SUN.
The question of the chemical con
stitution of the sun, and Its physical
state, whether solid, liquid or gaseous,
seemed but a few years since to be be
yond the reach of science. But in the
hands of skilled astronomers the spec
troscope has answered these and many
other Interesting questions. A brief
description of the principle of this
instrument will help In a measure to
understand how these results are ob
tained. If sunlight coming through a small
hole In a dark room passes through a
glass prism and tho light then falls on
a sheet of white paper, It will be
be found to be drawn out Into a rainbow-colored
band of light, red at one
end. violet at the other, with the rest
of tho colors between. This Is the
spectrum of sunlight. Examined, how
ever, merely as above described, the
spectrum is Impure, adjacent colors
overlap. By means of the spectro
scope this overlapping of colors Is pre
vented. This Instrument consists es
sentially of a narrow silt about one
one-thousandth ot an Inch wide, on
which the light to be examined falls,
a prism, usually of glass, which di
vides the light coming from the silt
into Its constituent colors, and a teles
cope fo4- examining tho light after
passing through the prism. By means
of such an instrument It Is founJ
that the light from a white-hot solid,
liquid, oi gaseous body, under great
pressure, always gives a continuous
spectrum, that is, an unbroken band
of oolor.s, n spectrum from which no
color Is missing. When, however, the
light of an Incandescent gas, such as
npodium, or magnesium flame, an
electric spark or an electric arc Is ex
amined, there is no cohtiuous spectrum
but instead a series of bright lines.
Every element gives Its characteris
tic bright line spectrum.
If now this incandescent gas be ex
amined against the brighter back
ground of a white-hot solid or li
quid pubstonce, hotter than the gas
there Is seen a continuous spectrum
Interrupted by dark lines which coin
cide exactly with the bright lines of
the gas. Now on examining sunlight
with the spectroscope, we find It has a
contluous spectrum, broken by m.inv
fine, dark lines, which coincide with
the lines of the spectra of a number
of Known terrestrial elements. Wo
may, therefore, confidently say that
that there elements are present In the
rnlar atmosphere ns Incandescent
E ises
How accurate this method Is will In
part appear fiom tho fact that the ele
ment helium was first found on tho
sun and only later traced to earth.
Among the elements discovered on the
sun are potassium, sodium, magnesium,
nickel, cobalt, calcium, silicon, tltanum
carbon, oxygen, copper, platinum and
Iron. Professor Rowland, who has
made an extensive study of the solar
spectrum, says that If the earth wero
heated as hlchlv as the sun It would
give precisely the same spectium,
TO THE EYE AND CAMERA.
Visual photographic observations of
the sun show that Its brightness de
creases from the center toward tho
limb, owing to the greater depth of
solar atmosphere through which the
latter Is seen. It Is found that less than
one-half as much light and heat as Is
radiated at tho center Is given oft at
the limb of the sun, ?ne action of
tho solar atmosphere Is found to be
similar to our own. Less of the violet
light penetrates It than of the red.
Under the Influence of tho Intensn
heat the sun's atmosphere Is kept In
a state of violent disturbance in com
parison with which Western cyclones
nnd West Indian hurricanes are mere
zephyrs. Two photographs of tho sun,
tho onn taken ten minutes after the
other, disclosed an evident change in
the solar surfuce, which, to ho detected
at all, oven under tho most favorable
conditions, Implied a motion of at least
47 miles.
Tho visible surface of the sun Is
called tho photosphere. Eamlned un-
-Wo atmospheric conditions
with ii special eyepiece to reduce the
blinding Intensity of the sun's Imago,
It Is found to be covered with minute
granules much brighter than the back
ground on which they lie, presenting
nn appearance which has been likened
to snowflnkes on a white sheet. These
granules nre bright Incandescent
clouds. Though they occupy less than
one-hnlf of the sun's surface, they
radiate most of Its light.
CHEMICALS IN THE SUN.
The layer of gas lying Just over tho
Photosphere to a depth of about COO
miles contains most of tho elements
which produce the dark lines In tho
solar spectrum, nnd lsfor that reason
called the reversing layer. Tho spec
trum of tho reversing layer photo
graphed In the absence of light from
the solar surface, as on the occasion ot
a totnl eclipse of the sun, consists ot
bright lines, the dark lines reversed.
Above the reversing lnycr Is the chro
mosphere, the sun's atmosphere of
which tho reversing layer Is the lower
lying strata. The chromosphere ex
tends from 5,000 to 10,000 miles above
the solar surface. It Is composed prin
cipally of hydrogen nnd helium. SeeSi
onlv on tho occasion of a. total eclipse
it presents to quote Professor Young
"the appearance of a scarlet flame, not
composed of horizontal sheets, but of
upright filaments. Its nppearanco has
been compared very accurately to a
prairie on fire." This, however, Is not
to bo understood to mean that com
bustion takes place. Tho temperature
Is too high for that.
In the chromosphcro are to bo seen
scarlet cloud-llko objects suspended
60,000 or 60,000 miles above the photo
Rphero, with which they are generally
connected by means of slender fila
ments. These are quiescent promi
nences. They are masses of lncnnde.
cent gases, principally hy.drogen and
helium. Other prominences arc to bo
seen which differ from the quiescent In
that they are much more brilliant and
active. They appear to be cast up from
the body of the sun by an explosive,
or eruptive force, and hence are called
eruptive prominences. They contain
many other metals besides hydrogen.
At times they change with astonishing
rapidity, having been observed to move
with velocities of 200 and 250 miles a
second.
Prominences are visible during a
total eclipse of tho sun with a tele
scope, and occasionally even to tho
naked eye, presenting the appearance
of crimson flames projecting from the
black disk of the moon. By means of
the spectroscope prominences may be
observed without an eclipse, and a
modified form of this instrument en
ables the nstronomer to photograph
them.
THE CORONA.
On the occasion of a total eclipse
there may be seen, nnd seen at that
time only, the silver bands and stream
ers of the corona extending radically
ftom the sun. Photographic and vis
ual observances of tho corona are
among the most Important that can be
made at a total eclipse. A compari
son of nccurato drawings with photo
graphs of the corona shows that the
two nro substantially the same In ap
pearance. The latter has tho advan
tage of furnishing a permanent and
accurate record not only of Its general
appeatance, but also of Its minute de
tails, and may bo studied at leisure
in tho laboratory. The form and size
of the corona, as well as Its bright
ness, change greatly. In general the
coronal streams are made up of bands
and filaments often strangely curved
and Intertwined. Near the poles they
resemble tufts of threads sharply de
fined. For tho most part tho length
of the streamers does not exceed the
sun's radius, but at times some ot
thtm arc seen to extend far out Into
space, as was observed In the clear
air of Colorado at the eclipse of tlSTS,
where two of them were traced to a
distance of 9,000,000 miles. Tho spec
trum In the corona shows that It
shines partly by reflected sunlight and
partly by light emitted by tho incan
descent gasses which compose it,
among which are calcium, hydrogen
nnd a hitherto unknown gas called
coronlum recently said to have been
discovered in Italy.
Tho ccrona Is formed of matter
ejected from tho suri. Us substance
must be Inconceivably lare, since
comets have passed through It with
out suffering a notlceabli- change In
their motion. All methods- heretofore
tiled for photographing or mapping
tho corona without an eclipse have
failed because of the brightness of our
atmosphere.
TO MEASURE LIGHT.
Among tho Interesting observations
to bo made Rt the coming eclipse will
be measurements of the Intensity of
the coronal light, tho distribution of
tho different rases In it by means of
tho spectroscope, the hent It radiates,
tho form of tho coronal streamers and
their variation In brightness at dif
ferent distances from tho sun. Spes
troscopes will bo used to photograph
r
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the spectrum of the 'reversing layer
nnd determine If possible, the distri
bution In altitude of the different
metallic gases and their probable tem
perature. Search will be made by
means of photographs taken In tho
neighborhood of tho sun to find it
thers bo any undiscovered planet ly
ing within the orbit of Mercury. Many
useful observations can be made by
amateurs and will, If found accurate,
be published by the United States gov
ernment. A pamphlet clvlng details
of useful observations, photographic
and visual, which may be made by
amateurs with little or no apparatus
can bo obtained on application to Cap
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the naval observatory, Washington, D.
C.
Not all pcllnsea are total. At times
tho moon passes to one side over tha
face of the sun; there is then a partial
eclipse. Again the apparent size of tho
moon may be smaller than that of the
sun, so that when seen centrally over
the solar disk tho dark disk of our
satellite Is surrounded by a bright rlni;
of tho sun's surface: this Is an annular
eclipse. Total and annular eclipses are
seen only over a comparatively narrow
belt of land and last at most for a few
minutes, but partial ecllpsss are seen
over a much wider extent of tho earth's
surface and last much longei. Tho
same eclipse which la total or annular
ulong but a narrow strip of the earth's
surface Is seen as a partial eclipse over
a much wider nrea.
THE DIFFDHENT ECLIPSES.
The distinction between tho different
eclipses may bo simply Illustrated by
holding between the eye and a globe
lamp a piece of circular cardboard, say
of half the diameter of the globe. The
shadow of the card may be divided
Into two parts; tho umbra, the shadow
cono converging to a point within
which all light from the lamp Is cut
off, the penumbra a shadow cono dl
verging outward surrounding the um
bra within It only a part of tho globs
Is visible. If tho eye be placed within
tho umbra tho globe cannot bo seen; It
Is totally eclipsed. Seen with tho oyo
placed In the axis of the umbra but
beyond Its apex In the penumbra a
bright ring Is seen; this Is an annular
eclipse.
We may, therefore, regard eclipse
thus: The moon always casts a shadow
in space consisting of the umbra, a
converging cone from which the sun's
light Is excluded, and a penumbra, a
diverging caso within which but a par
of the sun's surface may be seen. If
only the penumbra of tho moon's
shadow falls on tho earth there Is a
partial eclipse. The umbra may con
verge to a point beyond the earth or
fall short of It. If the axis of tho
umbra Intersects the earth, but Its
npex does not reach It, the eclipse Is
nnnular. If tho umbra Itself falls on
the earth the ecllpso Is total. It Is
because the moon's shadow Is so small
a diameter and moves so fast that n
total eclipse Is seen over so narrow n
belt of land and for so short u time.
As tho dark body of the moon en
croaches on the sun It cannot be seen
with the naked eye, until tho exposed
surface of tho sun Is reduced to a verv
thin crescent. Then suddenly this cres
cent la broken up into a string of
bright beads, named after tho astrono
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just the man we want to see. We feel
proud of these Ready-to-Wear Suits. We
want you to come here and examine the
cloth. Try one on and look at yourself
in our large "duplex" mirror.
1
$12
-$
finished with silk, bxcel- S
lpnr vnliin nt v
our fc
P
v.i iuiuv
er Bros
Scranton's Leading Outfitters.
mer who first described them as
Bailey's beads. They are duo to pro
Jectlng mountain peaks on tho limb ot
tho moon, which first cut the bright
crescent. From the distance is now
seen rushing with surprising swiftness
tho dark Bhadow of tho moon. Sud
denly tho sun's light vanishes, tho sum
shine out. nature is affected as if sur
prised by night, tho body ot tho moon
stands out black against the crimson
photosphere surrounded by the sllveiy
streamers of the corona. The eclipse
Is now total. Soon the moon moves off
tho sun, and a Hood of light from Its
brilliant surface drowns tho wondious
nnd beautiful spectacle.
OUR BEST PURCHASER.
Amount of Our Products Bought by
England nnd Her Colonies.
From the WasliIiiRton Star.
England buys CU per cent, of all tin?
products which the American farmer
sends abroad, says Consular Agent E.
L. Harris, at EIb?nstock, In a recuiit
report to tho htato department ti eat
ing upon tho extent of United States
trade with Great Urltuln. England, ho
says, Is our best customer for over
production in food scuffs, Mid tho
Ilrltish colonies present the greatest
field for out manufactured products.
Consular Agent Harris piovldes a ta
ble for the fiscal year, 1S9S-99, showing
that England bought, In round num
bers, 1711,000,000 worth of our principal
products, or 79 per cent, moro than all
the rest of Europe combined.
"This report," says Consular Agent
Harris, "is based upon tho statistics
published by tho Deutsche Kolonlal
zeitung, Bradstrevt'a annual report
and on a statistical abstract for tho
several colonics and other British pos
sessions IssiiPd In London. They are
figures which every farmer, manufac
turer and laborer in the United States
Bhould know. They are especially in
teresting when wo consider that the
English colonies nro not Included. The
farmers of our great central stutes
will see at a glance what the English
market means to iorn, wheat. Hour,
beef and pork. England buys CO per
cent, of all tho products which the
American farmer bends abroad. I may
add that Great Britain has never
shown the enmity toward these pro
ducts which has characterized the ac
tions of some European nations. The
cotton grower of the south la aware
of tl'o vuluo of tho English market
for his products. But the manufnc
turer of lion and steel has tho great
est Interest In tho British empire ns
a market. HIh exports to England
may be proportionately small, but in
the colonies ho is ndvanclng with
strides and bounds. He hun more to
hope for from these colonies In tho
future than from nny other countiies.
Our bridge builders nro busy In India
und Egypt. Our steel rails, machin
ery and galvanic wires are In South
Afrlcn, British enterprise and stabll- 1
Ity In nil these countiies means in- I
creased opportunities nnd marketH for
our manufacture!!!. The moro one be-
comes familiar with the continent of ,
Europe the moro one la satisfied that !
no lasting Jesuits can be obtained
here with manufactured articles. The
amount of labor spent in trying to
1
New
Cloth Styles In
Ready-to-Wear Suits
We compare the Ready-to-Wear
Suits in our 15 sale to
any custom tailor suit at $25.
We know it would be impossi
ble to make a single, suit and
give the same quality, cloth and
workmanship. See them dis
played in our Lackawanna ave
nue window. There you can
tind cloth patterns that
are not shown else
where in this city at
"Bon Bon" Underwear
In two weights, light and medium.
This underwear has a silky finish
and is the most comfortable for
summer wear. Regular made and
m.i........ .ii.
"
,'?)'TrV,--wr,'.p?,v"vr".?T.'P-'vT.!'''v?,ri,j'f,,!! .ilv'wt."' tj 'i
BEAUTIFUL
m a.
A Hf.ttlc of the Misses Hell's Ccle
hated Complexion Tonic Without Cost
This generous offer Is made in
order that ali may have an oppor
tunity to test its wonderful merits
Beauty's chief chirm is tho complex
ion. If the i-Uin 1st tear und smooth, a
woman will lie classed ns beaut 1 fill cvrn
If natiiio has not given htr pefect
LTho Misses Drl!, of 70 Fifth Avenue,
Nov York, when they placid their now
juilly lelibiatcd Complexion Tonic be
tore the public, g.ive to ihoio suffering
frm poor comphxicms a boon long
1 ceded, Tliouoiuuls have made their
kins absolutely pcifeci by its uc.
Mow, hi order to stlll'fuithcr Intro
duce It, the Jliv-cs Hull will give to any
luly wiltiug tlnin during tho present
month mi opportunity to tiy one large
Iiottlo (tho price of which is $1) (it
ii-o'ululy no cost. Do not wait, but
iU.ND AT ONCE.
Tho Mics Dell'' Complexion Tonio
N not u paint ot powder to cox or up Iho
fri'ikli'', pimples or moth patches, but
is, ns its nutno Implies, n tonic for tho
kiii. It rradiratcs tho blemish entirely
and forcvir. It not only dois this, but
it beautifies tho skin, smoothing away
wrinkles, drawing out ALL dlscolora
tions removing nil pimples, acne,
uc7cina or roughness,
Tho .Misses lUll hnvo nt their parlor!
uioio than ten ttiottviml letters fiom
parous ntkiiowlidging wonderful im.
provemfiiN in Ihur complexions. Tho
Mi-sen Hell havo never utd a testi
monial In public pilut.as they valuo a
woman's (Icllc.icy in such things, hut
tho oilgitml liitters can bo seen nny
timont pailots 70 Fifth Avenue.
Huiu'inbcrnn opportunity isglvcn you
to tivouo hottluof this really wonder
ful f onio for tho skin FREK. A-ldic.
THE MISSES BELL
76 Fifth Avenue, New York'City
aeuie maikets In France, Ocrjnnny
and other Europenn countries will
havo three nnd four-fold results In
Africa, Siberia, China, Australia and
South America. Cordial relations with
Otea: Britain will carry us many a
nilK'Htoni) nn the way We havo tlunis
uHdsi ot laboiera -and skllltd wotUmen
who are dependent for their existence
upon tho sale of our ovei production.
England Is bur best customer for over
production In food stuffs. The British
colonies present the greatest field, for
our manufactured products,"
mma 'jdSS
..- -