zodiac, it should therefore be possible to determine the sun's velocity relative to the aether, or at least that component of it which lies in the ecliptic.
The same principles may be applied to the discussion of other astronomical phenomena. Thus the minimum of a variable star of the Algol type will be retarded or accelerated by an interval of time which is found dividing the projection of the radius from the sun to the earth on the direction from the sun to the Algol variable by the velocity, relative to the solar system, of propagation of light from the variable; and thus the latter quantity may be deduced from observations of the retardation.[1]
Another instance in which the time taken by light to cross an orbit influences an observable quantity is afforded by the astronomy of double stars. Savary[2] long ago remarked that when the plane of the orbit of a double star is not at right angles to the line of sight, an inequality in the apparent motion must be caused by the circumstance that the light from the remoter star has the longer journey to make. Yvon Villarceau[3] showed that the effect might be represented by a constant alteration of the elliptic elements of the orbit (which alteration is of course beyond detection), together with a periodic inequality, which may be completely specified by the following statement: the apparent coordinates of one star relative to the other have the values which in the absence of this effect they would have at an earlier or later instant, differing from the actual time by the amount
,
where m1, and m2 denote the masses of the stars, c the velocity of light, and z the actual distance of the two stars from each
- ↑ The velocity of light was found from observations of Algol, by C. Y. L. Charlier, Öfversigt af K. Vet.-Ak. Förhandl, xlvi (1889), p. 523.
- ↑ Conn. des Temps, 1830.
- ↑ Additions à la Connaissance des Temps, 1878: an improved deduction was given by H. Seeliger, Sitzungsberichte d. K. Ak, zu München, xix (1889), p. 19.
