LATITUDE OBSERVATIONS

• Document Type: CREST
• Collection: General CIA Records
• Document Number (FOIA) /ESDN (CREST): CIA-RDP80-00809A000600200259-4
• Release Decision: RIPPUB
• Original Classification: R
• Document Page Count: 6
• Document Creation Date: December 22, 2016
• Document Release Date: June 29, 2011
• Sequence Number: 259
• Publication Date: September 2, 1948
• Content Type: REPORT

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ace whose iy has bean asocrta?smd.
s
an emmple of how one station can control the whole world should there be
established at that eta+ion a lcrgi.tuda service or a universal azimuth (der-
vice, in addition to latitude obsezvationa. This means that from 6bser atiom;
conducted at this station a corresponding 4/P`, which' is necesosry for doj..or
mining the mean latitude q;, may be obtained for any point of the cari;h o svr
f
In one of AV works `3j I mentioned the Graarniich latitude stat4o , a
s !Ambers in brackets refer to the bibliograr,472
In addition, i, will. be abaolutel?r related to the ono and the some polar
mean (the origin of the (yatem of right,-angle coordinates) chocot arbit-arily
I this Atgt4
6n
.
The system of an independent ;,Quiet latitude servfoe, which dooo not re-
quire fKarimtional cooperation and catch I doai?,:od to bring to the attuntiot,
of Soviet astronomers, is based. on this.
Based on currant cothrds (other conCitions being ocual), and in view of
the feasibility of using cimpior instruments (telescopes :ritbout hors?.ontal.
t
i
urn
ng axon), it is my o)iniou that only 50 percent of the capital noo(led to
equip a ooirec onding ]at-1 .ado service is nsaeled to realize this system.,
For the salve of brevity, I later on refer to the usual determinations
of a latitude as absolute, according to which observations of stars are con-
duoted whoa the zenith telescopc is placed in two positioi.a. In order ':n
detbrmine variations in the latit,xie, 19u,',,gw;t, that the staro be observed
without a resottirlg of the instr cent and the results of such obsorvationa be
called relative dotwulnations of latitude.
CLASSiFIC4TION L E iTKICTTsD
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RD137C
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PLACE
ACQUIRED
DATE OF
IN ORMATION 1948
CENTRAL INTE NC- '9ENC,,
D;1TE DISiR.2
NO. OF PAGES
NO. OF ENCI.S.
(LISTED BELOW)
SUPPLEMENT TO
REPORT NO.
epi:ember 1918
6
STAT
STAT.
OT THE fifth ittlt3 ?1111011 t01 0ftf0110 or us WHOOA0l ACT SO
0. 1. C.. 01 ?1O 00. U ?0111000. NS TOAM/010/IOM OR TVt !!V[MTIOO
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CO 006520 SOCWCW1 IT tmt 00(010000 ROW-
'THIS IS UNEVALUATED INFORMATION FOR THE '2ESEARC14
USE OF TRAINED INTELLIGENCE ANALYSTS
SOURCE Russian periodical, ' .8 1 m3 ,1 1, 1949. (rib Per Abe ;aT6
Translation specifically requested.
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' Inoonne.otion.-lt1? ciao Sw_otlatitudc- 3:r7=co, c;;orJetion: shoral:.1 ho
conducted at least at tn'o station.
One station (the main station), in addition to observing the absolute
and relative determinations of latitude, is engaged in azimutbal determination
of one polar coordinate (y), vtila the second station (substation) limits
itself to the relative determination of latitude and azimuthal determination
ofethe second polar coordinate (x).
Azimuthal determination of polar coordinates, apparently being nerd
easily realizable than longitud5xml locations of polar coordinates, is
specified in the system I suggeiited.
The difference in longitudes of the abovo-montioned stations should be
as close as possible to 90 degrees so that reductions to an ideal rsaridian
euld be close to zero.
In order to avoid netting up stations in net places, it is possible, in
my opinion, to limit ourselves to combinations of Pulkovo-Irkutsk or even
Poltava-Irkutsk stations. Reductions of these stations to the meridian A.
270 degrees -- for the p e of obtaining (wy) according to the formulas
L
1.] result in the foiiouing:
in Tables 2, 10, and 1
Pulkovo (min station.3 a (X) 01), Irkutsk (substation it = 2860 o )
For latitudinal observations r270 =-O.'27(=.- 0.039y
For longitudinal obserationa r270 a -0.05( ,- O.356Y
For asimutbal observations r270 s 0.064x 0.4515
Poltava (main station s a co0'), Lrkutsk (substation A 29001J.
For latitudinal observations rr270
?0.346x
o.csb2y
For longitudinal observations 7r 70
_ -0.0ECz
4- 0.14cy
For azimuthal observations ;1r270
0.101x
-. 0.565Y
Hero, 7 and y are arbitrary designations for the polar coordinates.
It saust be noted that even though the prosenee of a substat! a is riot
required, it is apparently very desirable because its existence insures the
possibility of checking results of the determinations of the polar coordinator
obtained by various methods.
If the meridian of the main station is tnkea as the primary-neridion,
and if bhe vest longitude of ins substation is equal sa 2700, the ?ollorring
ip.1P.+X,
aaao theses eP
on the basin of Qbich, obsorvatione of the rain station are expressed iL the
follasving manner on the polar coordinates:
14 a ko"' - 9-oacosq' (azimuthal deterairs'Mon of the polar
u.: a,~ t X J c
ocordizBtes)
On the bases of the fol]oring equations
x i = Y;' + If, - (Po relative determination of the latitude) t2)
STAT
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terry latitude and mean latitude; a and so, momentary and mean azlrch of the
universe, respectively; Ms, point of zonith; and c%-, an average reading of
the micrometer adjusted to the inclimation of the vertical axis, curvatwo of
the parallels and refraction and declination of the bair, providing the ob-
servations are conducted by the hour angle method. If observations of stars
are made with fixed hairs, adjustments must be made for a collimation error
(azimuthal determination of polar coordinates) (4)
Y'' - `P. - (`Q' f,1) (relative determination of latitude)
'Clan fo7J.c;!iu;;; co?t:ol vain arc cbtaLicdfro;.-Lob, at:a,io: conducted by tb
substation according to formula (9) cited in
Thus, the formula for relative dotormdmtion of altitude unuat road:
In this instance and Al are invariable qunniities.
so Chet the origin of the coordinatoo mould coincide an olozely as possible
with the polar moan used in international laticudr sarvdco. If gush values
are leaking, we may confine ourselves to the following formula (5).
for q, and o. (in cozmeotion pith oqw-tiona (1) cud (2)) at the min station
im the `P;, r~., and A
T -' (T MIS ~IIO.Y ~j .u'rJ :; 4 ?(a/iV } Qnt ../ ~. (S)..
.
pressed in the following ?orLpila after proper observations, of ai by'the sub-
taaeous detormiaationa of dif'fororcee
At the substation, ao, which enters into equations (3) and (4), is
z; mow; r:s .
Two mesa should be disti.nguishod ..ben oatablizbilig
N. - J, w! (7)
1) mien the value of 4'? is laical;.
In this instance c f', -44, j - f (C)
2) When the value of q is not given.
forms:
+ (9)
That is to any, observations of c are distinguished from the valve (-yi)
by an invariable quantity (W -Nz), the value of Jhich may be found by the
main station with the aid corresponding values of yi, by using the following
u3-
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A 49. 1 P ' S P , ! d A /1,, and 4 a. s a - ' o) are
eatabliahocl (vitll the aid of known equations (10)) for any point on the
earth's our oo then the Clout longitude, which is relative to the main eta-
The factors noceeoary for ocmot location of googratahio coordinates,
pinging the aslautbal method.
the rolativo method; and 3) Oro aeries of values for the pair (xi,, ?Pi) by em-
ne aeries of vslaxas for ` th? pair (xi, 9'i) by employing
absolute method; 2)"On
a ce = x CoS A t R
4 A (x ~~a A Y-4 A) zar, cfr j 6 0w : Cy o.s A - A JhN A) sec f
0b?q a 0 A T71gtSR~3nte
1ng 3W T .U un+~cnaraaaw.. .
vision abould be controlled by eonaitive overheadlovole. it isydesirayb]o
gn
es
t
e
strtnaent, equipped with an ocular nioromator ;7hich is
f ic"MMY Poll awful, t olowep 3
firmly and permanently attached to a atone pillar so that the line of vision
of the telescope would be vertical, vin probably be sufficient for obtain
ed
The lama app
in this case observations of stars arc conducted nithout rsaottingthe in-
of the instxammnt Gan be greatly simplified. A euf-
b
d
i
to the relative determinations of latit des. Sines
li
ALM P....e... itll zenith tEllesG617ee must be
zenith stare singly or in pairs. Only apetl
used in observations (instr mnta aimilar se installed in Greemrioh
and ostersborg or models suggested by me ,L2 2j.
.W
In alb U JJ U0 J 'U
polar eoor+.ivatee with the beir' of the mooromotor set on Polaris during its
All senith stars vitbin the reach of the telescope should be observed.
its lino of vision set on Polaris.
In this case the tolesoopo should be mounted in such a msnioor as to
OX Ti'A p7JJar, aau wa i a+ama
wed Zor absolute latitudinal observation., it Is-ne eauary 7 to~provJ deter a re, -
para nith_a depression on ITS tipper suns . -......r.a.. ..- ?_.. .
__ft_ -aa._.t.A +.. +l.s ..eA+nwn And agatern sides
prfaaalO14 on LIF7 O4lsu.ro L
so t t Its leO of Vialon could bo 4etod 'w *Uw Ucrt St .eaY::, arrange-
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The ocular micrometers of the above-mentioned te.Y.oaoopea can be replaocd
easily with either moveable or ? zed adapters for Aejtographic platen. The
place is occupied by a cotmtearwi[?,nt.
observation, t7hioh can be transported from the mein station for temporary
eontrol observations, is foreseen. In the aboeneo of t %U toloacope:, its
Two telescopes ore mounted on a same kind of foundation at the sub.
ntatIon. The poseibi ity of setting up a third teleacoce for absolute
0 81*10 formulae.
In the event that there are two min stations, the convorsion from a
fixed polo of one station to that of the other station is done with the aid
periodically, and then or]y to chnoI the position of Nln.
aeivioc, the basic equipment oeasiata of a pavi111on t7ith n usa33ve stone
pillar to which thine 6- to 7-inch telescopes are scoured at the main station
and a similar pavillion with two tel:oecopea at the substation.
In oonolvaton, I could like to dram attention to the following. If it
ni 1beipaasible to inctvU a teloecopo for detormining ho relative locations
of a latitude so nootmate17 the Sim 17311 become a sufficiently invsr_idule
quantity, the n%d for a regular deteridnation of absolute locations of a
latitude tvfll then be ollminetod. It nil]. o%37 be neoesoary to do; thin
alert W 0, 9G, 190, and 2700, ~s; na~ew) 64 V,4,',' t1 "`,!
fiotitious meridian, the fol3oving has been abt{i3md for longittdes, equiv- r..
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1. V. K. Abend, "A Pier for the Reorganization of the International
Latitude 5ervioo," Astro. . Vol 24, No 5, 1947
2. V. K. Abol'd, "On the Aoouracy of LatitWes Located by the Telflotta
Method Based on . observations of Zenith Stars and Pairs of Stara: A
Plan for a SPeo3a1 Zenith Telaaoopo," AotroAatro_ Zurn. Vol 16, Tb 1, 1939
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