Page:Encyclopædia Britannica, Ninth Edition, v. 23.djvu/380

Rh and A" 4, &c., so that all the A"s are to be found in terms of K z, which is known, and of K 4, which is apparently indeterminate. The condition for the convergency of the series (34) for u and for the series du/dv is that K K+ ilK-x shall tend to a limit less than unity. The equation (35) may be written AT2144_2i-f3 _____ K&,gg&amp;gt; AVh2~2i + 6 2i(2i + 6) AW" Now A^+2/ A*2i tends to be either infinitely small or not infinitely small. If it be not infinitely small in the limit, the second term on the right of (36) becomes evanescent when i is very great, and we have in the limit when i is very large V=flBut the ratio of successive terms of /(l ~ " ) tends to become (l-f/i&amp;gt; 2 . Hence, if K^^Ky. does not tend to become infinitely small, u = A + BVl -v 2, where A and B are finite for all values of v. Again, under the same circumstances we have in the limit when i is very large .A 1 V, 3 A 1 4 + l But the ratio of successive terms of (I-? 2 ) ~* tends to (1 -/i) 2 Hence, if Kx+n/Ka does not tend to become infinitely small, duldv = C + D(l - 1- 2 )"*, where C and D are finite for all values of v. XT da ^ u i o~ /~( /i i T Now -j3=-r Vl- 2 = Cvl-i 2 + D. dO dv Therefore at the equator, where v = l, dn/d6 = D, a. finite quantity. Hence the hypothesis that AVi-2/^2 tends to be not infinitely small leads to the conclusion that u and dn/d& are finite at the equator. But on account of the symmetry of the system the co-latitudinal displacement must vanish at the equator, and therefore x also. By (23), when/=l, k=2, y = sin 0, But we have just seen that this hypothesis makes u finite when / =! or 0=90, and therefore at the equator 1 du _ ., ... x = -;—,-r, a finite quantity. 4m d& Now symmetry necessitates a vanishing value of du/dO at the equator. Thus the hypothesis that A 2,-+2/^2i tends to be not in finitely small is negatived, and we conclude that, on account of the symmetry of the motion, it is infinitely small for infinitely great values of i. This being established, let us write (36) in the form Hence by repeated application of (36a) we have And we know that this is a continuous approximation to A" L _ which must hold in order that the latitudinal velocity may vanish at the equator. Writing N, = AT^+a/ K^, all the N s may be com puted from the continued fraction (37). Then We cannot compute K 6 from AT 4, A g from AT 6, and so on; for, if we do, then, short of infinite accuracy in the numerical values, we shall be gradually led to successive values of the K s which tend to equality. 1 This process was followed by Laplace without explanation. It was attacked by Airy in his " Tides and Waves " (in Ency. Metrop. ) and by Ferrel in his Tidal Researches (U.S. Coast Survey, 1873), but was justified by Sir W. Thomson in the Phil. Mag. (1875, p. 230). The investigation given here is substantially Thomson's. Solu- Laplace gives numerical solutions for three different depths of lions. the sea, -3-5^, T^*S-, sa 1 ts f the earth's radius. Since tn~^^, these correspond respectively to the cases of =40, 10, 5, and the solutions are =40, h = E{v 2 + 20-1862v 4 + 10 1164i 6 - 13 1047 8 -15-4488y 10 -7-4581i/ 12 - 2-1975? 14 - 4501i 16 - O-OeS?? 18 -0-0082V 20 - 0-0008? 22 - O OOOlc 24 ...} =10, h = E{i&amp;gt; 2 + e-igeOi 4 + 3-2474c 6 + 07238 8 + Q-QVlQv 10 + 0-0076p 12 + 0004v 14 ...} = 5, h = E{v 2 + 0-7504J/ 4 + 0-1566i/ 6 i Thomson calls this a dissipation of accuracy. It may t&amp;gt;e illustrated thus. Consider the equation 2-31+2=0, which may be written either z=j+Jx 2 or x= 3 - 2/x. Now let x tt+l = + Jj: 2,^ and suppose we start with any value XQ, less than unity, and compute xj, 3%,. . . x n. Then, starting with x n in the equation x n _ l =3-Z/x n, if we work backwards, we ought to come to the original value zo. In fact, however, we shall only do so if there is infinite accuracy in all the numerical values. For, start with &o=i. then Zi = -75, a%2= 8542, z 3 =-9099, a; 4 = -9527, 5 = 9692; and the values go on approximating to 1, which is a root of the equation. Next start backwards with x 5 = -97, and we find z 4 = -938, 3= -868, z. 2 = -696, x l = -l-27,x = - 1275, x_ l =3~157, x_ 2 =2 367, z_ 3 =2-155, x_ 4 = 2-072; and the values go on approximating to 2, the other root of the equation. Since h vanishes when v = 0, there is no rise and fall of water at the poles. When v = 1 at the equator, we find =40, h=-7 434E = 10, h = 11-267E = 5, h= 1-924E. The negative sign in the first case shows that the tide is inverted at the equator, giving low water when the disturbing body is on the meridian. Near the pole, however, that is, for small values of v, the tides are direct. In latitude 18 (approximately) there is a nodal line of evanescent semi-diurnal tide. In the second and third cases the tides are everywhere direct, increasing in magnitude from pole to equator. As diminishes the tides tend to assume their equilibrium value, because all the terms, save the first, become evanescent When =1 (depth 7 of radius) the tide at the equator still exceeds its equilibrium value by 11 per cent. As diminishes from 40 to 10 the nodal line of evanescent tide contracts round the pole, and when it is infinitely small the tides are infinitely great. The particular value of for which this occurs is that where the free oscillation of the ocean has the same period as the forced oscilla tion. The values chosen by Laplace were not well adapted for the illustration of the results, because in the cases of =40 and = 10 the depth of the ocean is not much different from that value which would give infinite semi-diurnal tide. For values of greater than 40 we should find other nodal lines dividing the sphere into regions of direct and inverted tides. We refer the reader to Sir W. Thomson's papers for further details on this interesting point.

In treating these oscillations i^aplace remarks that a very small amount of friction will be sufficient to cause the surface of the ocean to assume at each instant its form of equilibrium, and he adduces in proof of his conclusion the considerations given below. The friction here contemplated is such that the integral effect is represented by a retarding force proportional to the velocity of the water relatively to the bottom. Although proportionality to the square of the velocity would probably be nearer to the truth, yet Laplace's hypothesis suffices for the present discussion. In oscillations of this class the water moves for half a period north, and then for half a period south. In oscillating systems, where the resistances are proportional to the velocities, it is usual to specify the resistance by a modulus of decay, namely, that period in which a velocity is reduced to c" 1 of its initial value by friction. Now the friction contemplated by Laplace is such that the modulus of decay is short compared with the semi-period of oscillation. The quickest of the important tides of long period is the fortnightly (see chapter iv.); hence, for the applicability of Laplace's conclusion, the modulus of decay must be short compared with a week. Now it seems prac tically certain that the friction of the bed of the ocean would not materially affect the velocity of a slow ocean current in a day or two. Hence we cannot accept Laplace's discussion as satisfactory. How ever this may be, we now give what is substantially his argument.

Let us write 6 for the reciprocal of the modulus of decay. Then the frictional forces introduced on the left-hand side of (17) are + Gd%/dt in the first and sin OSdij/dt in the second. Laplace's hypothesis with regard to the magnitude of the frictional forces enables us to neglect the terms d-/dt- and sinQd^y/dt- compared with the frictional forces. Then, if we observe that in oscillations of this class the motion is entirely latitudinal, equations (17) and (19) become

dt +2n cos 0=0 dt dt sin + j(y sin 6)

From the first two of these we easily obtain

q d. (, 4?r g+ ^ (38). .(39).

As a first approximation we treat d/dt as zero, and obtain I)=r, or the height of water satisfies the equilibrium theory. In these tides (see chap, iv.) f = I (J-cos 2 0) cos it, so that from the third equation of (38) we can obtain a first approximation to |; then, sub stituting in (39), we obtain on integration a second approximation to h. Laplace, however, considers as adequate the first approxima tion, which is simply the conclusion of the equilibrium theory.

As it seems certain that these tides do not satisfy even approximately the equilibrium law, we now proceed to find the solution where there is no friction. In the case of these tides k= O,/ a small fraction, and e = E (^-cos 2 0). The equation (24) then becomes