LADING WORKS, AND FURNISHING DATA FOR THE CONSTRUCTION OF MODELS-DETERMINING COMPARATIVE ALTITUDES WITH THE MOUNTAIN BAROMETER, &c. The method of ascertaining the difference of level between stations on a trigonometrical survey by means of reciprocal angles of elevation and depression observed with a theodolite, has already been alluded to in page 30; and sections of ground can be taken in the same manner, though not so accurately as with a spirit-level. It is however necessary first to explain two corrections that must be applied to vertical angles, particularly when observed for the purpose of obtaining relative altitudes on an extended triangulation between stations a long distance apart. If they are only separated by a few hundred yards, these corrections are too trifling to have any appreciable effect on the result. Considering the earth as a sphere, any number of points on its surface equi-distant from its centre are on the same true level; but the apparent level, and of course the apparent altitude, or depression, is vitiated by the two causes of error alluded to,—Curvature and Refraction; the corrections for which depend upon the arc contained between the stations. The effect of the curvature of the earth is to depress the apparent place of any object. Every horizontal line is evidently a tangent to a the surface of the globe at that spot; and the difference between the apparent and true level at any distant station B (putting the effects of refraction out of the question for the present) will be seen, by reference to the figure, to be the excess (x) of the secant of the arc AD above the radius. P t A 2 ? a2 Putting a for the arc AD, t for the tangent AB (the horizontal line, or line of apparent level), r for the radius AC, or DC, and x for the excess of the secant BC above the radius or the difference between the true and apparent level. Then (r + 2) 702 + t2. Whence x (2r + x) = t'; and owing to the small proportion that any distance measured on the surface must bear to the earth's radius, 2r may be substituted for (2r + x), and the arc a, for the tangt. t; 2 r x then becomes= a’, and x = 2r, which, assuming the mean diameter of the earth at 7916 miles, gives x = 8.004 inches or .667 of a foot for one mile; which quantity increases as the square of the distance. Or otherwise, 2r + X :t::t: X, or 2 r : a :: a : x. x being omitted in the expression (2r + x) and a substituted for t; whence x = as before. 2r A very easily remembered formula, derived from the above, for the correction for curvature in feet, is two-thirds of the square of the distance in miles ; and another, for the same in inches, is the square of the distance in chains divided by 800.* The second correction, Terrestrial Refraction, on the contrary, has the effect of elevating the apparent place of any object above its real place. The rays of light bent from their rectilinear direction in . passing from a rare into a denser medium, or the reverse, are said to be refracted; and this causes an object to be seen in the direction of the tangent to the last curve at which the bent ray enters the eye, as in the figure below: a2 * The amount of the correction for curvature at different distances, will be found L A is any station on the surface of the earth, the sensible horizon of which is AB; C and D are two stations on the summits of hills, of which C is supposed in reality to be situated on the horizontal line AB, and D above it, the angle of elevation of which is BAS. Owing, however, to the effects produced on the rays from these objects in their passage to the eye by the atmosphere through which they pass, they are seen in the directions As and A b, tangents to the curve described by the rays, and BA b, and SA s, are the respective terrestrial refractions. Above eight or ten degrees of altitude, the rate at which the effects of refraction decrease as the altitudes increase, is so well ascertained, with the variation depending upon the temperature and density of the atmosphere, that the refraction of the heavenly bodies for any altitude may be obtained with minute accuracy from any of the numerous tables compiled for the purpose of facilitating the reduction of astronomical observations; but when near the horizon, the refraction, then termed terrestrial refraction, is so unequally influenced by the variable state of the atmosphere, that no dependence can be placed upon the accuracy of any tabulated quantities.* The rays are sometimes affected laterally, and they have been even seen convex instead of Periods for observing angles of depression and elevation, particularly if the distances between the stations are long, should therefore be selected when this extraordinary refraction is least remarkable; morning and evening are the most favourable, and the heat of the day after moist weather, when there is a continued evaporation going on, is the least so. It is a common custom to estimate the effects of refraction at some mean quantity, either in terms of the curvature, or of the arc of distance. The general average in the former case is 4 of the curvature, making the correction in feet for curvature and refraction combined = 4 Do, # , D being the distance in miles, as before. In the latter the proportion varies considerably; † and General Roy, in the opera concave. by reference to the tables, and further remarks on Atmospheric Refraction in the chapter on the Definitions of Practical Astronomy. # Puissant “ Geodesie,” vol. i. page 342; and “ Recherches sur les Refractions Extraordinaires par Bist.” Also, the “ Trigonometrical Survey,” vol. i. F. 352. + Carr's "Synopsis of Practical Philosophy;" articles, ‘Levelling,' and 'Refraction.' D a tions of the trigonometrical survey, assumed it at jó, and sometimes at 11, in cases where it had not been ascertained by actual observation of the reciprocal angles of elevation or depression, by the following simple method. These angles should, to insure accuracy, be observed simultaneously, the state of the barometer and thermometer being always noted: * In the accompanying figure, C represents the centre of the earth, A and B the true places of two stations above the surface SS; AD,BO are horizontal lines at right angles to the radii AC, BC; a and b are also the apparent places of A and B. In the quadilateral AEBC, the angles at A and B are right angles, therefore the sum of the angles at E and C are equal to two right angles; and also equal to the three angles, A, E, and B of the triangle AEB; taking away the angle E com-mon to both, the angle C, or the arc SS, remains = EAB + EBA; or, in other words, the sum of the reciprocal depressions below the horizontal lines AD, BO, represented by AEB + EBA, would be equal to the contained arc if there was no But a and b being the apparent places of the objects A and B, the observed angle of depression will be DA b, OB a; therefore their sum taken from the angle Cot (the contained arc of distance) will leave the angles b AB, a BA, the sum of the two refractions; hence, supposing half that sum to be the true refraction, we have the following rule when the objects are reciprocally depressed. Subtract the sum of the two depressions from the contained arc, and half the remainder is the mean refraction : If one of the points B, instead of being depressed be elevated, suppose to the point 9, the angle of elevation being gAD, then C REFRACTION. 66 * “ Trigonometrical Survey,” vol. i. p. 175. See also, on this subject, Woodhouse's Trigonometry,” p. 202. | One degree of the earth’s circumference is, at a mean valuation, equal to 365,110 feet, or 69.15 miles and one second=101.42 feet. the sum of the two angles, e AB and EBA, will be greater than EAB + EBA (the angle C, or the contained arc) by the angle of elevation, e AD: but if from e AB + EBA, we take the depression OB a, there will remain e AB + a BA, the sum of the two refractions; the rule for the mean refraction then in this case is, subtract the depression from the sum of the contained arc and the elevation, and half the remainder is the mean refraction.* The refraction thus found must be subtracted from the angle of elevation as a correction, each observation being previously reduced, if necessary, to the axis of the instrument, as in the following example, taken from the Trigonometrical Survey :-At the station on Allington Knoll, known to be 329 feet above low-water,t the top of the staff on Tenterden steeple was depressed by observation 3' 51", and the top of the staff was 3.1 feet higher than the axis of the instrument when it was at that station. The distance between the stations was 61,777 feet, at which 3.1 feet sultend an angle of 10'.4, which, added to 3' 51", gives 4' 1.'4 for the depression of the axis of the instrument, instead of the top of the staff. On Tenterden steeple, the ground at Allington Knoll was depressed 3' 35" : but the axis of the instrument, when at this station, was 5.5 feet above the ground, which subtend an angle of 18."4: this, taken from 3' 35", leaves 3' 16”.6 for the depression of the axis of the instrument. * The formula given in the “ Synopsis of Practical Philosophy,” is identical with this rule : (A +E)—D. Refraction .E being the apparent elevation of any height; D the 2 apparent reciprocal angle of depression; and A the angle subtended at the earth's centre by the distance between the stations. + A difference of opinion exists as to the zero from which all altitudes should be numbered. What is termed “Trinity datum,” is a mark at the average height of highwater at spring-tides, fixed by the Trinity Board, a very little above low-water mark at Sheerness. Again, some engineers reckon from low-water spring-tides; and as the rise of tide is much affected by local circumstances, this latter must, in harbour, and up such rivers as the Severn, where the tide rises to an enormous height, be nearer to the general level of the sea. One rule given for obtaining the mean level of the sea, by reckoning from low water-mark, is to allow one-third of the rise of the tide at the place of observation. At 206,265 feet distant, 1 foot subtends 1''; or at one mile it subtends 39.06 nearly. |