Account of a Voyage of Discovery Part 14

REMARKS ON THE OBSERVATIONS MADE WITH IT IN HIS MAJESTY'S SLOOP LYRA.

In our tables for apparent dip of the visible horizon at different heights from the sea, as calculated from the known curvature of the earth, allowance is made for the refraction of the atmosphere, on a supposition of its being constant, but as it is known to vary, the tabular dip will often be erroneous, and, consequently, alt.i.tudes taken under different states of the atmosphere, will exhibit different instead of corresponding results.

It is foreign to the present purpose to shew what the causes are which have most effect in raising or depressing the apparent horizon. It may be sufficient to mention, that changes in the relative temperature of the air and the sea must produce changes in the refraction near the surface. Dr. Wollaston has published two papers in the Philosophical Transactions on this subject, in the volumes for 1800 and 1803, and to these I beg to refer the reader for precise information upon this very curious subject.

The object which this sector proposes to attain, is the actual admeasurement of the dip angle; that is, to ascertain how much the visible horizon is depressed below the horizontal plane pa.s.sing through the eye of the observer. The instrument is so contrived as to measure double the dip angle twice over, so that we obtain four times the required dip, and one quarter of this angle is what must be applied to vertical angles, measured from that part of the horizon which has been observed.

Figure I. is the instrument seen in perspective, and Fig. II. is a plan of it with the telescope removed. In order to explain its use, let A and B (Fig. II.) represent the two reflecting gla.s.ses at right angles to the plane of the instrument, and also nearly at right angles to each other.

It is clear that when the plane of the instrument is held vertically, an eye situated at E, and looking through the unsilvered part of the gla.s.s A at a distant point C, will at the same time see by joint reflection from both gla.s.ses, another distant point D at 180 from C; and D will appear to correspond with C, if a suitable motion be given to the index gla.s.s B by the tangent screw F.

The instrument may now be supposed to measure the arc CZD. If the points C and D be each three minutes farther from the zenith than 90, the entire angle will then exceed 180 by double that quant.i.ty. The relative position of the gla.s.ses then corresponds to 180 6', and the six minutes of excess would be shewn on the arc at F if there were no index error.

But, by reason of the index error, the real quant.i.ty will not be known till a similar observation has been made with the instrument in an opposite direction.

If the instrument be now inverted, so that the unsilvered gla.s.s is uppermost, the arc intended to be measured is CND, or the sum of the distances of the points C and D from the Nadir instead of the Zenith, which of course falls short of 180 by as much as the former arc exceeded that quant.i.ty.

The difference of the two arcs is consequently twelve minutes, and if the index be now moved till the objects C and D appear to correspond, the amount of this double difference will be shewn by the _change of position_ of the vernier.

Hence it is evidently unnecessary that the index error should be previously known, and even preferable that its amount should be such as to avoid the needless introduction of negative quant.i.ties by positions on different sides of zero.

In the preceding description, it is supposed that the eye is looking directly through the unsilvered gla.s.s at the horizon, and that it also perceives the opposite horizon after two reflections; but an inspection of the figure will shew that the observer's head would necessarily intercept the rays from the horizon behind him. To obviate this, both the direct and the reflected rays are received in coming from the unsilvered gla.s.s, (and after pa.s.sing through the field-gla.s.s of the telescope) on a mirror placed at an angle of 45, which reflects them to the eye. By this ingenious contrivance, the obstruction is removed, and the opposite points of the horizon may be both seen at one moment.

In practice, it is most convenient to direct the telescope to the same part of the horizon in both cases. Thus, if the east and west parts of the horizon be observed, and that the index gla.s.s be uppermost, and telescope pointing to the west, the observer is on the south side, and his face must be turned to the north. When the instrument is inverted, if the observer turn himself round at the same time, so as to face the south, then the telescope will be pointed as before to the west; but since the index gla.s.s is now undermost, the inferior arc will now be measured precisely as if his face were to the north, but with the advantage of the same lights seen in the erect position of the instrument.

In using this instrument at sea for the first time, considerable difficulty arises from the constant change in the plane of the instrument from the perpendicular position, in which it is absolutely necessary that it should be held, in order to obtain a correct observation. What at first appears to be a defect, however, is a real advantage, namely, that whenever it is held in the least degree out of the vertical plane, the two horizons (that seen direct, and the reflected one) cross each other, and it is only when the plane is vertical that the horizons can appear parallel.

The object is to get the two horizons to coincide exactly, and for this purpose it will often be necessary to have them of different shades.

This is managed, as in the s.e.xtant, by means of the screw, which raises or lowers the telescope. When the telescope is brought nearer to the plane of the instrument, the reflected horizon becomes dark and distinct, but when screwed off it becomes fainter, and is not so well defined. Practice alone can teach the degree of intensity which is most favourable. In general it is best to have one horizon dark, and the other light; then bring them very nearly to coincide, and wait till the s.h.i.+p is steady, at which moment a slight touch of the tangent screw brings them exactly to cover one another. It will happen, of course, that when the coincidence is perfect, there is only one horizon to be seen, and a doubt remains whether all is right, but a slight motion of the instrument, by making the horizons cross each other, defines them at once.

It is advisable to take several observations, and the safest way is to take one first with the index gla.s.s uppermost, and then with the instrument inverted, after which to return to the first, and so on for two or three times each way.

In the pages which follow, there is given a table containing the result of all the observations made during this voyage, preceded by several sets of observations in the fullest detail. From the table it will be observed how seldom the dip, actually measured, agrees with that inferred from the mean refraction. Some of these experiments shew very remarkable differences, and point out the great utility of this instrument.

The practical navigator, particularly if he has been in hot climates, will recollect how discordant his observations for lat.i.tude always were, and how few even of the best observers agree in their determination of the lat.i.tude of the same place, simple as the observation is thought to be. The cause is quite clear; and though it equally affects alt.i.tudes taken for absolute time, the disagreement is less obvious, and it will often happen that a chronometer going extremely well appears to vary every day from inaccuracy in the observations. Thus it is, I think, generally admitted, that it is almost impossible to rate a chronometer from alt.i.tudes observed with the sea horizon. Nor is this difficulty removed by taking equal alt.i.tudes, because the refraction in all probability will be different at the two observations. With an artificial horizon, indeed, the changes in refraction are not felt, because, at a considerable elevation above the horizon, the changes are very trifling. But it often happens in practice, that the artificial horizon cannot be used, and we are then reduced to the sea horizon, where the changes of refraction are always the greatest. In the Yellow Sea, for instance, we had no opportunity of landing during all the time that the squadron was at anchor, till the day before we sailed. So that during nearly a fortnight that the s.h.i.+ps were at anchor, the sea horizon was necessarily used. I need only to refer to the observations taken off the Pei-ho, viz. from No. 37 to 62, to shew how extremely fallacious the results must have been.

It is much to be wished that this excellent instrument should be brought into general use in navigation.

THE FOLLOWING EIGHT OBSERVATIONS ARE SET DOWN IN THE FULLEST DETAIL, IN ORDER TO SHEW THE METHOD USED IN RECORDING THEM.

No. 31.

YELLOW SEA.

_July 23, 1816._--6 P.M.

Index uppermost. Instrument inverted.

A + 8'. 10" B - 7'. 10"

8 . 05 7 . 10 8 . 00 7 . 10 ------ ------ Mean 8 . 05 Mean 7 . 10 B.

Mean + 8 . 05 A.

------- 15 . 15 ------- 3 . 49 Dip.

3 . 50 Tabular.

1 Difference.

Height of the eye, 15 feet, 3 inches.

Parts of the horizon observed, WSW. and ENE.

Barometer 29 . 78 inches Thermometer {Air 82 {Sea 77 Lat.i.tude 35 north.

Longitude 124 east.

Wind light from south; horizon uncommonly well defined and sharp; sky clear, and sea perfectly smooth.

No. 40.

OFF THE PEI-HO, YELLOW SEA.

_July 29, 1816._--9 A.M.

Index uppermost. Instrument inverted.

A + 8'. 20" B - 11'. 40"

8 . 45 11 . 35 8 . 30 11 . 50 ------ ------- Mean 8 . 32 Mean 11 . 42 B.

Mean + 8 . 32 A.

------- 4) 20 . 14 5 . 3 Dip.

3 . 50 Tabular.

1 . 13 Difference + -------

Height of the eye, 15 feet, 3 inches.

Parts of the horizon observed, NW. and SE.

The low land just visible in the NW. distant 12 or 14 miles.

Depth of the sea, 18 feet.

Barometer 29 . 60 inches.

Thermometer {Air 81 {Sea 84 Lat.i.tude 38. 50' north.

Longitude 118. 00' east.

There has been little wind this morning, after a very close night.

No. 43.

OFF THE PEI-HO, YELLOW SEA.