The dark blue circle represents the ideally spherical surface of the Earth's ocean; the solid blue ellipse shows the result of tidal stretching. The height of the ellipse above the spherical surface, at P, is proportional to the vertical component of the solar tideproducing force at P. 
The Sun's gravitational field, since it stretches matter in the direction of the Sun, will deform the ideally spherical surface of the Earth's oceans into an ellipsoid of revolution, with major axis pointing towards the Sun. For the volume of the oceans to remain constant, the surface of this ellipsoid must lie alternately above and below the spherical surface. Let us define the ``solar tideproducing force" F at any point to be the vertical distance from the spherical surface to the stretched one. The figure shows that distance to be proportional to cos 2A(t), i.e. at a maximum when A(t) = 0^{o} or A(t) = 180^{o}: when the Sun is straight up or straight down.
Using the expression we have for A(t), this gives F proportional to cos (2 arccos LC{cos Tt, cos [T+2h]t, sin ht}). The identity cos (2 arccos x) = 2 x^{2} 1 yields:
= LC{ 1, cos^{2}Tt, cos^{2}[T+2h]t, sin^{2}ht, cos Tt cos[T+2h]t, cos Tt sin ht, cos[T+2h]t sin ht}.
A vigorous application of the trigonometric identities
The solar tideproducing force at a point P is, as a function of time, a finite linear combination of cosines and sines, whose speeds are certain integral linear combinations of T and h. 
The coefficients depend on the latitude of P.

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