STANDARD - Survey Instrument Antique Center!
STANDARD - Survey Instrument Antique Center!
STANDARD - Survey Instrument Antique Center!
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78<br />
To Find the Meridian from " Polaris."<br />
The north star, Polaris, being out of the pole of the equator, is in the meridian but<br />
twice in a stellar day once above and once below the pole called the upper and<br />
lower transits, or culminations.<br />
It is also at its extreme distance, east and west, twice in a stellar day, called<br />
greatest elongations, east or west.<br />
At the time of a culmination, it would be only necessary to get the bearing of the<br />
star to have the place of the true meridian. But this would require an exact knowledge<br />
of the time, an element not usually possessed by surveyors. Moreover, the<br />
observation must be made with certainty, at the instant, which is not always practicable.<br />
On this account, this method is not in favor with surveyors.<br />
At elongation, the apparent motion of the star is tangent to the vertical, and<br />
therefore, for a few minutes, with regard to azimuth, it appears to stand still, thereby<br />
Wording ample time for deliberate observation.<br />
The distance of thrs star from the pole- called its polar distance, was 1 18' 16"<br />
on January 1, 1885, and is diminishing at the rate of about 19.06" per year, whence<br />
its distance in following years may be known.*<br />
The azimuth of the star, corresponding to any polar distance, is variable with the<br />
latitude. Thus, an observer at the equator would see this star say at eastern<br />
elongation in the horizon, and at the distance of 1 18' 16" to the right of the pole,<br />
or true meridian.<br />
If now the observer should go north, the azimuth of the star would increase with<br />
its altitude, till he should arrive at a latitude equal to the complement of the polar<br />
distance, when it would be N. 90 E. Between these limits, the bearing of the st?,r,<br />
at elongation from the pole, would vary according to the following equation, in which<br />
Z = the azimuth, or bearing :<br />
.<br />
7 _ sin Polar Distance<br />
:<br />
cosine Latitude<br />
As the telescope of the surveyor's transit is not usually of sufficient power to show<br />
the star in the daytime, the observation must be made at night, in which case the<br />
cross-wires of the telescope must be illuminated by light reflected into the tube. A<br />
piece of stiff white paper, with an opening large enough to admit of seeing the star<br />
through it, and held obliquely in front of the telescope, will make a good reflector.<br />
As generally but one of the elongations can be seen, on the same night, it is important<br />
to know, which one is observed. Also the latitude must be known, at least<br />
approximately.<br />
The pole is nearly in line between Polaris and the star Mizar, which is at the bend<br />
in the handle of the Dipper, so that when these two stars are nearly in a horizontal line<br />
and the dipper is ^jjj. j-<br />
of the pole, Polaris is at his greatest elongation ^J j-<br />
In sighting to the star, the observer must be careful to keep his transit level<br />
transversely, for the star is so high that inattention to this might introduce a serious<br />
error into the resulting azimuth.<br />
A satisfactory sight having been obtained, the telescope should be brought down<br />
to fix a mark on the ground, at a distance of 300 to 400 yards from the transit.<br />
This mark should be something clear and definite, like a nail set in a hub, driven<br />
into the ground, which may be located by means of a plummet lamp, or by means<br />
of a common lamp in a box, having a vertical slit in one side of say or f an inch in<br />
thickness, with a plumb-line suspended from the slit, and manipulated by an<br />
assistant.<br />
The direction of the star being satisfactorily marked, compute the azimuth from<br />
1<br />
the above equation, and set the resulting angle off to the I<br />
?,. ] of the mark for<br />
It may happen, that the resulting azimuth may have an odd number of seconds,<br />
or fraction of a minute, not convenient to be set off with a vernier graduated to<br />
* Small corrections to the distances thus calculated are needed, but do not amount to more than 30" IB<br />
all ; see a Nautical Almanac.